15th HEAD Naples, FL – April, 2016 Meeting Program Session Table of Contents 100 – AGN I Analysis Poster Session 206 – Early Results from the Astro-H 101 – Galaxy Clusters 116 – Missions & Instruments Poster Mission 102 – Dissertation Prize Talk: Accretion Session 207 – Stellar Compact II driven outflows across the black hole mass 117 – Solar and Stellar Poster Session 300 – The Physics of Accretion Disks – A scale, Ashley King (KIPAC/Stanford 118 – Supernovae and Supernova Joint HEAD/LAD Session University) Remnants Poster Session 301 – Gravitational Waves 103 – Time Domain Astronomy 119 – WDs & CVs Poster Session 302 – Missions & Instruments 104 – Feedback from Accreting Binaries in 120 – XRBs and Population Surveys Poster 303 – Mid-Career Prize Talk: In the Ring Cosmological Scales Session with Circinus X-1: A Three-Round Struggle 105 – Stellar Compact I 200 – Solar Wind Charge Exchange: to Reveal its Secrets, Sebastian Heinz 106 – AGNs Poster Session Measurements and Models (Univ. of Wisconsin) 107 – Astroparticles, Cosmic Rays, and 201 – TeraGauss, Gigatons, and 304 – Science of X-ray Polarimetry in the Neutrinos Poster Session MegaKelvin: Theory and Observations of 21st Century 108 – Cosmic Backgrounds and Deep Accretion Column Physics 305 – Making the Multimessenger – EM Surveys Poster Session 202 – The Structure of the Inner Accretion Connection 109 – Galactic Black Holes Poster Session Flow of Stellar-Mass and Supermassive 306 – SNR/GRB/Gravitational Waves 110 – Galaxies and ISM Poster Session Black Holes 400 – AGN II 111 – Galaxy Clusters Poster Session 203 – Missing Baryons and the Hot Halo of 401 – The Unique Role of Very High 112 – Gamma-Ray Bursts Poster Session the Milky Way Energy Observations in Multi-Wavelength 113 – Gravitational Waves Poster Session 205 – Plenary Talk: Observation of Astronomy 114 – Isolated Nss Poster Session Gravitational Waves in Advanced LIGO, 402 – Dark Matter, ISM, & Galaxies 115 – Laboratory Astrophysics and Data Laura Cadonati (Georgia Tech) 403 – Rapporteur Plenary Talk imaging and polarimetry can give us clues to the locations of the 100 – AGN I radiating particles in each band, as well as their kinematics and the jet's structure. We discuss new work that describes how 100.01 – An HST proper-motion study of the optical observations in several bands can be knit together to form a more jet in 3C 264: Direct Evidence for the Internal Shock coherent picture of jet physics. Model Some of the most energetic phenomena in the Universe involve Author(s): Eric S. Perlman1, Sayali S Avachat1 , Devon highly relativistic flows, in which particles are accelerated up to TeV Clautice1332 , Markos Georganopoulos , Eileen Meyer , Mihai Cara energies. In the case of relativistic jets from Active Galactic Nuclei Institution(s): 1. Florida Institute of Technology, 2. Space (AGN), these flows can carry enough energy to significantly Telescope Science Institute, 3. UMBC influence both galactic and cluster evolution. While the exact physical mechanism that accelerates the radiating particles within 100.03 – New insights into AGN coronae the jet is not known, a widely adopted framework is the internal Active galactic nuclei (AGN) are some of the most energetic sources shock model, invoked to explain high-energy, non-thermal of radiation in the Universe. The conversion of gravitational energy radiation from objects as diverse as microquasars, gamma-ray into radiation is thought to take place in an accretion disk/corona bursts, and relativistic jets in AGN. This model posits an unsteady system just outside the black hole. In this system thermal, relativistic flow that gives rise to components in the jet with UV/optical photons from the accretion disk are upscattered in a different speeds. Faster components catch up to and collide with corona of hot electrons situated above the accretion disk producing slower ones, leading to internal shocks. Despite its wide popularity X-rays. The nature of this Comptonizing corona remains a key as a theoretical framework, however, no occurance of this open question in AGN physics. The NuSTAR satellite provides the mechanism has ever been directly observed. We will present opportunity to study the Comptonization spectrum produced by evidence of such a collision in a relativistic jet observed with the the corona in great detail. In our talk we will show some key results Hubble Space Telescope (HST) in the nearby radio galaxy 3C 264 from these new studies of the Comptonization spectrum. We (Meyer et al., 2015, Nature). Using images taken over 20 years, we explore how, together with our growing knowledge of coronal sizes, show that a bright ‘knot’ in the jet is moving at an apparent speed of we are able to draw first conclusions about the physics taking place 7.0 +/- 0.8c and is in the incipient stages of a collision with a in the corona. We find evidence for coronae to be hot and slow-moving knot (1.8 +/- 0.5c) just downstream. In the most radiatively compact, putting them close to the boundary of the recent epoch of imaging, we see evidence of brightening of the two region in the compactness–temperature diagram which is knots as they commence their kiloparsec-scale collision. This is the forbidden due to runaway pair production. This suggests that pair behaviour expected in the internal shock scenario and the first production and annihilation are essential ingredients in the direct evidence that internal shocks are a valid description of coronae of AGN and that they control the coronal temperature and particle acceleration in relativistic jets. shape of the observed spectra.

Author(s): Eileen T. Meyer4, Markos Georganopoulos4 , Author(s): Anne Lohfink2, Andrew C Fabian21 , Julien Malzac , William B. Sparks31 , Eric S. Perlman , Roeland P. Van Der Marel 3 , Renaud Belmont12 , Douglas Buisson Jay Anderson32 , S. Tony Sohn , John A. Biretta 3 , Colin Arthur Institution(s): 1. Universite de Toulouse, 2. University of Norman23 , Marco Chiaberge Cambridge Institution(s): 1. Florida Institute of Technology, 2. Johns Hopkins University, 3. Space Telescope Science Institute, 4. 100.04 – Chandra solves the mystery: Understanding University of Maryland, Baltimore County the UV anomaly discovered by HST A strange anomaly was discovered during our 180 day HST 100.02 – Multiwavelength Observations of AGN Jets: campaign to observe NGC5548 for reverberation mapping. The UV Untangling the Coupled Problems of Emission emission lines responded to changes in the UV continuum, as they Mechanism and Jet Structure should, during most of The discovery of X-ray and optical emission from large numbers of the observing season. However, there was a period of about 60--70 AGN jets is one of the key legacies of the Chandra X-ray days during which the UV emission lines decorrelated from Observatory and Hubble Space Telescope. Several dozen optical continuum variations. Understanding this anomaly is vital to the and X-ray emitting jets are now known, most of which are seen in success of reverberation mapping technique. We also observed the both bands as well as in the radio, where they were first discovered. source 4 times with Chandra during the 180 day HST observations. Jets carry prodigious amounts of energy and mass out from the Chandra observations revealed the presence of soft excess during nuclear regions out to tens to hundreds of kiloparsecs distant from the anomaly, but there was no soft excess before or after the the central black hole, depositing it into the host galaxy and cluster. anomaly. This suggests that the accretion disk temperature Interpreting their multiwavelength emissions has not been easy: increased from the ``normal'' state, peaking in FUV, to that while in most jets, the optical and radio emission in many objects is peaking in soft X-rays during the anomaly. Thus, there was no believed to emerge via the synchrotron process, due to its ionizing continuum to which to reverberate. There are more characteristic spectral shape and high radio polarization, the X-ray curious things about the response of emission lines, such as the emission has been a tougher nut to crack. In less powerful, FR I time at which the anomaly sets in and the amount flux decrease jets, such as M87, the X-ray emission is believed to be synchrotron during the anomaly. I will discuss the details of this first-of-its-kind emission from the highest energy electrons, requiring in situ behavior and present detailed explanation. particle acceleration due to the short radiative lifetimes of the particles. However, in FR II and quasar jets, a variety of emission Author(s): Smita Mathur1, Anjali Gupta1 mechanisms are possible. Until the last few years, the leading Institution(s): 1. The Ohio State University interpretation had been inverse-Comptonization of Cosmic Microwave Background photons (the IC/CMB mechanism). This 100.05 – A New Look at Ionized Disk Winds in requires the jet to be relativistic out to hundreds of kiloparsecs Seyfert-1 AGN from the nucleus, and requires an electron spectrum that extends to very low Lorentz factors. However, that now appears less likely, We present an analysis of deep, high signal-to-noise due to observed high optical polarizations in jets where the optical Chandra/HETG observations of four Seyfert-1 galaxies with known and X-ray emission appears to lie on the same spectral component, warm absorbers (outflowing winds), including NGC 4151, as well as limits derived from Fermi observations in the GeV MCG-6-30-15, NGC 3783, and NGC 3516. Focusing on the 4-10 gamma-rays. It now appears more likely that the X-rays must arise keV Fe K-band, we fit the spectra using grids of models as synchrotron emission from a second, high energy electron characterized by photoion- ized absorption. Even in this limited population. With this revelation, we must tackle anew the coupling band, the sensitive, time-averaged spectra all require 2-3 zones between jet structure and emission mechanisms. Multiwavelength within the outflow. In an improvement over most previous studies, re-emission from the winds was self-consistently included in our weak enough to allow KHI rolls unsuppressed. Our simulation, models. The broadening of these emission components, when tailored to the specific scenario, will provide further insight into the attributed to Keplerian rotation, yields new launching radius details of the transport process. estimations that are largely consistent with the broad-line region. If this is correct, the hot outflow may supply the pressure needed to confine clumps within the broad-line region. NGC 4151 and NGC Author(s): Ralph P. Kraft1, Yuanyuan Su11 , Paul Nulsen , Elke 3516 each appear to have a high-velocity component with speeds Roediger213 , William R. Forman , Eugene Churazov , Christine comparable to 0.01c. The winds in each of the four objects have Jones11 , Scott W. Randall , Marie E. Machacek 1 kinetic luminosities greater than 0.5% of the host galaxy Institution(s): 1. Harvard-Smithsonian, CfA, 2. Hull University, bolometric luminosity for a filling factor of unity, indicating that 3. MPA they may be significant agents of AGN feedback. 101.02 – Exploring the Outskirts of the Galaxy Cluster Author(s): Allison Bostrom1, Jon M. Miller1 Merger A1750 Along the Putative Large-Scale Filament Institution(s): 1. University of Michigan The entropy profiles in the outskirts of clusters generally fall below the self-similar prediction based on purely gravitational models of 100.06 – Relativistic reverberation in the accretion hierarchical cluster formation. Weakening accretion shocks and flow of a Tidal Disruption Event the presence of unresolved cool gas clumps, both of which are Our current understanding of the curved spacetime around expected to correlate with large-scale structure filaments, are supermassive black holes is based on actively accreting black holes, among the possible interpretations of observed entropy flattening. which make up only ten per cent or less of the overall population. A1750 is a triple merger system, with all three subclusters lying X-ray observations of that small fraction reveal strong gravitational roughly along the same line, suggesting the presence of large-scale redshifts that indicate that many of these black holes are rapidly structure filament. Our recent Suzaku and Chandra X-ray, and rotating, however selection biases suggest that these results of a MMT optical observations of the early stage galaxy cluster merger few are not necessarily reflective of the majority of black hole spins A1750 show that entropy profiles at the cluster's virial radius are in the Universe. Tidal disruption events, where a star orbiting an self-similar and gas mass fractions are consistent with the mean otherwise dormant black hole gets tidally shredded and accreted on cosmic value both along and perpendicular to the putative large to the black hole, can provide a short, unbiased glimpse at the scale filament. These results may suggest that gas clumping is less spacetime around the other ninety per cent of black holes. prevalent in lower temperature and mass clusters. I will also Observations of tidal disruptions have hitherto revealed the describe the properties of the cool (< 1 keV) gas detected at large formation of an accretion disc and the onset of an accretion- cluster radii along the filament direction, which is consistent with powered jet, but have failed to reveal gravitational redshifts from the expected properties of the denser, hotter phase of the WHIM. innermost regions close to the event horizon, which enable the measurement of black hole spin. Here, we report observations of Author(s): Esra Bulbul5, Scott W. Randall44 , Matthew Bayliss , reverberation arising from photons from highly ionized iron (from Eric Miller543 , Felipe Andrade-Santos , Ryan Johnson , Mark W. K shell electrons) reflected off the accretion flow in a tidal Bautz524 , Elizabeth L. Blanton , William R. Forman , Christine disruption event. The asymmetric iron line profile indicates that we Jones464 , Rachel Paterno-Mahler , Stephen S. Murray , Craig L. are seeing a region close to the event horizon of the black hole, Sarazin741 , Randall K. Smith , Cemile Ezer where gravitational redshifts are strong. From the reverberation Institution(s): 1. Bogazici Univ, 2. Boston Univ., 3. Gettysburg time delay, we estimate the mass of the central black hole to be a College, 4. Harvard-Smithsonian Center for Astrophysics, 5. MIT, few million solar masses. Combined with the observed luminosity, 6. University of Michigan, 7. University of Virginia we conclude the tidal disruption event is accreting at least 100 times the Eddington limit, which is consistent with predictions of 101.03 – AGN feedback in the Perseus cluster the mass fallback rate of a tidally disrupted star. The detection of Deep Chandra images of the Perseus cluster of galaxies have reverberation from the relativistic depths of this rare hyper- revealed a succession of cavities created by the jets of the central Eddington event demonstrates that the X-rays do not arise from supermassive black hole, pushing away the X-ray emitting gas and the relativistically moving regions of a jet, as previously thought. leaving bubbles filled with radio emission. Perseus is one of the rare examples showing buoyantly rising lobes from past radio Author(s): Erin Kara1, Jon M. Miller2 , Christopher S. outbursts, characterized by a steep spectral index and known as Reynolds11 , Lixin J. Dai ghost cavities. All of these structures trace the complete history of Institution(s): 1. University of Maryland, 2. University of mechanical AGN feedback over the past 500 Myrs. I will present Michigan results on new, ultra deep 230-470 MHz JVLA data. This low-frequency view of the Perseus cluster will probe the old radio- emitting electron population and will allow us to build the most 101 – Galaxy Clusters detailed map of AGN feedback in a cluster thus far. 101.01 – A Deep Chandra Observation of NGC 1404: Author(s): Marie-Lou Gendron-Marsolais4, Julie Hlavacek- the Best Constraints on the Transport Processes in Larrondo4213 , Tracy E. Clarke , Huib Intema , Andrew C Fabian , the Intracluster Medium Gregory B. Taylor56 , Katherine Blundell The intracluster medium, as a magnetized and highly ionized fluid, Institution(s): 1. Leiden Observatory, Universiteit Leiden, 2. provides an ideal laboratory to study plasma physics. We present Naval Research Laboratory, 3. University of Cambridge, 4. results from the Chandra X-ray observation of NGC 1404, a bright University of Montreal, 5. University of New-Mexico, 6. University elliptical galaxy falling through the ICM of the Fornax Cluster. The of Oxford hot, gaseous corona surrounding NGC 1404 is characterized by a sharp upstream edge and a downstream gaseous tail. We resolve 101.04 – Microphysics of intracluster plasma with an the scales of contact discontinuities down to an unprecedented X-ray microcalorimeter level due to the combination of the proximity of NGC 1404, the Our usual assumption of a Maxwellian distribution for thermal superb spatial resolution of Chandra, and a very deep (670 ksec) electrons in the intracluster plasma may be incorrect, as evidenced exposure. We observed Kelvin-Helmholtz instability (KHI) rolls by in-situ observations in the solar wind plasma. Strong deviations and put an upper limit on the viscosity of hot cluster plasma. We are possible, and even likely, in cluster locations where cosmic ray also observed a mixing between the hot cluster gas and the cold acceleration should be occurring as seen from the resulting galaxy gas in the downstream stripped tail, providing further synchrotron radio emission, such as radio halos and relics. Recent support of a low viscosity plasma. Across the upstream front, we theoretical work shows that such non-Maxwellian electron measured a discontinuity smaller than the mean free path. The distributions would alter the ionization balance and emission line magnetic field is strong enough to suppress electron diffusions but ratios for various elements, and even the shape of thermal continuum that we use for cluster temperature determination. The core-collapse; (3) put the most stringent constraints to the Astro-H microcalorimeter will be able to detect such deviations if progenitors of Type Ia SNe by using the deepest X-ray observations the bulk of the intracluster plasma is non-Maxwellian, and future ever obtained. (4) Reveal the ejection of a massive stellar envelope high angular resolution microcalorimeters will be able to study timed with the collapse of a stripped star. These observations such deviations at shock fronts, radio relics and other special represent the first solid detection of a young extragalactic stripped- locations. envelope SN out to high-energy X-rays of ∼40 keV

Author(s): Maxim L. Markevitch2, Lynn Wilson2 , Thomas W. Author(s): Raffaella Margutti1 Jones54 , Dongsu Ryu , Gianfranco Brunetti 13 , Siang P. Oh Institution(s): 1. New York University Institution(s): 1. IRA/INAF, 2. NASA GSFC, 3. UCSB, 4. UNIST, 5. Univ. Minnesota 103.02 – Observational Constraints on the Supernova Engine 101.05 – Kinetic Modeling of Electron Conduction- Over the past 4 decades, the proposed engine behind normal Driven Microinstabilities and Their Relevance for core-collapse supernova has evolved considerably with increasingly AGN Feedback detailed models. These models produce increasingly firm Since the Intracluster Medium (ICM) is a weakly collisional predictions of the nature of these explosions. Unfortunatley, there plasma, the standard Spitzer conduction rate (which relies on is a level of indirection connecting these predictions to actual collisionality) does not necessarily describe the transport of heat in observations. Here we review the current observational constraints clusters. In addition, many plasma microinstabilities become on the supernova engine (and its underlying physics). unstable at high beta since the magnetic field is easily pliable in the presence of induced pressure anisotropies. These properties imply Author(s): Chris Fryer1 that the true rate of conduction in an ICM-like plasma could be Institution(s): 1. LANL highly dependent on small-scale effects. We perform 2D kinetic Particle-In-Cell simulations and derive an analytic theory of a 103.03 – Flares from stars tidally disrupted by conduction-driven electron microinstability present in high-beta supermassive black holes collisionless plasmas. We find that scattering by electromagnetic Stellar tidal disruption events are unique probes of accretion waves significantly reduces the conductive heat flux of electrons in physics and disk winds under extreme conditions. Their luminous our model. Our results have implications for 1) cool-core clusters in flares of radiation are signposts of intermediate-mass black holes which AGN feedback may play a crucial role in maintaing overall (BHs) and recoiling BHs. In X-rays, they have the potential to thermodynamic stability, 2) heat flux suppression and scattering by probe GR effects near the last stable orbit. Some of the events other microinstabilities and 3) basic plasma physics questions that launch relativistic jets, and provide us with a powerful new method up until this point have not been explored fully. of understanding the physics of jet formation and evolution in a quiescent environment. About 30-40 candidate events have been Author(s): Gareth Roberg-Clark1, M. Swisdak1 , Christopher identified by now, mostly in the X-rays and the optical. Events will S. Reynolds11 , James Drake be detected in the thousands in upcoming sky surveys, enabling Institution(s): 1. University of Maryland, College Park statistical studies and rapid multi-wavelength follow-ups. Here, I provide a review of the field, including most recent results. 102 – Dissertation Prize Talk: Accretion Author(s): St. Komossa1 Institution(s): 1. Max-Planck-Institut fuer Radioastronomie driven outflows across the black hole mass scale, Ashley King (KIPAC/Stanford 103.05 – Explorer for Transient Astrophysics: an University) X-ray transient mission for the 2020s Explorer for Transient Astrophysics (ETA) is a wide-field X-ray 102.01 – Accretion driven outflows across the black transient mission proposed for flight starting in 2023. Through its hole mass scale unique imaging X-ray optics that allow a 30 deg by 20 deg FoV in -11 Pumping highly relativistic particles and radiation into their three separate modules, a 1 arc min position resolution and a 10 2 environment, accreting black holes co-evolve with their erg/(sec cm ) sensitivity in 2000 sec, ETA will observe numerous surroundings through their powerful outflows. These outflows are events per year of X-ray transients related to compact objects, divided into highly collimated, relativistic jets and wide-angle including: tidal disruptions of stars, supernova shock breakouts, winds, and are primarily associated with a particular accretion neutron star bursts and superbursts, high redshift Gamma-Ray states. Understanding just how these outflows couple to the Bursts, and perhaps most exciting, X-ray counterparts of accretion flow will enable us to assess the amount of energy and gravitational wave detections involving stellar mass and possibly feedback that is injected into the vicinity of a black hole. During supermassive black holes. The mission includes an IR Telescope this talk, I will discuss our studies of both stellar-mass and that allows on-board redshift determination of gamma-ray bursts, supermassive black hole outlfows, and how the similarities of these and a small gamma-ray burst monitor to be contributed by the flows across the mass scale may point to common driving Technion (Israel Institute of Technology.) mechanisms. Author(s): Jordan Camp1 Author(s): Ashley L. King1 Institution(s): 1. NASA/GSFC Institution(s): 1. KIPAC/Stanford University 103.06 – Time Domain X-ray Astronomy with "All-Sky" Focusing Telescopes 103 – Time Domain Astronomy The largest and most diverse types of temporal variations in all of astronomy occur in the soft, i.e. 0.5 to 10 keV, X-ray band. They 103.01 – Young Supernova explosions in the X-rays range from millisecond QPO’s in compact binaries to year long and hard X-rays flares from AGNs due to the absorption of a star by a SMBH, and X-ray observations are providing critical insights into Supernova the appearance of transient sources at decadal intervals. Models explosions and the nature of their progenitors. In this talk I will predict that at least some gravitational waves will be accompanied highlight some recent results from our dedicated programs at by an X-ray flare. A typical GRB produces more photons/sq. cm. in high-energies that allowed us to (1) uncover the weakest engine- the soft band than it does in the Swift BAT 15 to 150 keV band. In driven SNe and understand their link to Gamma-Ray Bursts; (2) addition the GRB X-ray fluence and knowledge of the details of the monitor the high-energy emission from shock energy deposition onset of the X-ray afterglow is obtained by observing the seamless into the stellar envelope as early as a few days after the onset of transition from the active burst phase that has been attributed to internal shocks to the afterglow phases that has been attributed to (1+z). These findings are consistent with population synthesis external shocks. Detecting orphan X-ray afterglows will augment models, which attribute the increase in LMXB and HMXB scaling the event rate. With high sensitivity detectors some GRB relations with redshift as being due to declining host galaxy stellar identifications are likely to be with the youngest, most distant ages and metallicities, respectively. These findings have important galaxies in the universe. Previous all-sky X-ray monitors have been implications for the X-ray emission from young, low-metallicity non focusing limited field of view scanning instruments. An galaxies at high redshift, which are likely to be more X-ray “All-Sky” (actually several ster FOV), focusing lobster-eye X-ray luminous per SFR and play a significant role in the heating of the telescope will have much more grasp than the previous intergalactic medium. instruments and will allow a wide range of topics to be studied simultaneously. Two types of lobster-eye telescopes have been Author(s): Bret Lehmer11, Antara Basu-Zych6 , Stefano proposed. One type focuses in one dimension and uses a coded Mineo58 , W. Niel Brandt , Rafael T. Eufrasio 111 , Tassos Fragos , mask for resolution in the second. The other type focuses in two Ann E. Hornschemeier68 , Bin Luo , Yongquan Xue 14 , Franz E. dimensions but has less effective area and less bandwidth. Both Bauer95 , Marat Gilfanov , Vassiliki Kalogera 72 , Piero Ranalli , types are compatible with a Probe mission. Donald P. Schneider8133 , Ohad Shemmer , Paolo Tozzi , Jonathan R. Trump812144 , Cristian Vignali , JunXian Wang , Mihoko Yukita , Author(s): Paul Gorenstein1 Andreas Zezas10 Institution(s): 1. Harvard-Smithsonian Center for Astrophysics Institution(s): 1. Geneva Observatory, 2. IAASARS, 3. INAF, 4. Johns Hopkins University, 5. MPA, 6. NASA GSFC, 7. Northwestern, 8. Penn State, 9. Pontifica Catolica de Chile, 10. 104 – Feedback from Accreting Binaries in SAO, 11. University of Arkansas, 12. University of Bologna, 13. University of North Texas, 14. University of Science and Cosmological Scales Technology of China 104.01 – Accreting binary population synthesis and 104.04 – Studying the first X-ray sources in our feedback prescriptions Universe with the redshifted 21-cm line Studies of extagalactic X-ray binary populations have shown that the characteristics of these populations depend strongly on the The cosmological 21-cm line is sensitive to the thermal and characteristics of the host galaxy's parent stellar population (e.g. ionization state of the intergalactic medium (IGM). As it is a line star-formation history and metallicity). These dependencies not transition, a given observed frequency can be associated with a only make X-ray binaries promising for aiding in the measurement cosmological redshift. Thus upcoming next-generation radio of galaxy properties themselves, but they also have important interferometers, such as HERA and SKA, will map out the 3D astrophysical and cosmological implications. For example, due to structure of the early Universe. This 21-cm signal encodes a weath the relatively young stellar ages and primordial metallicities in the of information about the first galaxies and IGM structures. In early Universe (z > 3), it is predicted that X-ray binaries were more particular, X-ray sources in the first galaxies are thought to have luminous than today. The more energetic X-ray photons, because heated the IGM to temperatures above the CMB temperature, well of their long mean-free paths, can escape the galaxies where they before cosmic reionization. The spatial structure of the 21-cm are produced, and interact at long distances with the intergalactic signal during this epoch of X-ray heating encodes invaluable medium. This could result in a smoother spatial distribution of information about the X-ray luminosity and spectral energy ionized regions, and more importantly in an overall warmer distributions of the first galaxies. I will review this exciting new intergalactic medium. The energetic X-ray photons emitted from fronteer, highlighting how the 21-cm line will provide us with a X-ray binaries dominate the X-ray radiation field over active unique opertunity to study high-energy processes inside the first galactic nuclei at z > 6 - 8, and hence Χ-ray binary feedback can be galaxies. a non-negligible contributor to the heating and reionization of the Author(s): Andrei Mesinger1 inter-galactic medium in the early universe. The spectral energy Institution(s): 1. Scuola Normale Superiore distribution shape of the XRB emission does not change significantly with redshift, suggesting that the same XRB subpopulation, namely black-hole XRBs in the high–soft state, dominates the cumulative emission at all times. On the contrary, 105 – Stellar Compact I the normalization of the spectral energy distribution does evolve 105.01 – New Insights from Phase-Resolved with redshift. To zeroth order, this evolution is driven by the cosmic star-formation rate evolution. However, the metallicity Spectroscopy of QPOs in GX 339—4 evolution of the universe and the mean stellar population age are We present a new spectral-timing technique for phase-resolved two important factors that affect the X-ray emission from spectroscopy of low-frequency Type B quasi-periodic oscillations high-mass and low-mass XRBs, respectively. In this talk, I will (QPOs) from the black hole X-ray binary GX 339--4. Evidence review recent studies on the potential feedback from accreting suggests that low-frequency QPOs originate from near-periodic binary populations in galactic and cosmological scales. geometric changes in the inner accretion flow, possibly due to Furthermore, I will discuss which are the next steps towards a more general relativistic precession. The physical model predicts spectral physically realisitc modelling of accreting compact object energy distribution changes on the QPO timescale, but it is not populations in the early Universe. possible to probe these changes using strictly spectral or timing analysis. Our new technique shows that for these data, the spectral Author(s): Tassos Fragos1 energy distribution changes not only in normalization, but in Institution(s): 1. Geneva Observatory, University of Geneva spectral shape also, on the QPO timescale. We find that a blackbody spectral component and power law spectral component are both 104.02 – X-ray Evolution of Normal Galaxies in the 6 required to vary on the QPO timescale, and the blackbody Ms Chandra Deep Field-South variations are out of phase with the power law. With these findings we suggest a geometry for the precessing flow in the strong-gravity I will discuss recent efforts to quantify the evolution of X-ray regime close to black holes. binary (XRB) populations through cosmic time using the 6 Ms Chandra Deep Field-South (CDF-S) survey. The formation of XRBs Author(s): Abigail L Stevens1, Phil Uttley1 , Michiel van der is sensitive to galaxy properties like stellar age and metallicity--- Klis1 properties that have evolved significantly in the broader galaxy Institution(s): 1. University of Amsterdam population throughout cosmic history. I will show that scaling relations between X-ray emission from low-mass XRBs (LMXBs) 105.02 – Detection of Quasi-Periodic Oscillations in with stellar mass (LX/M) and high-mass XRBs (HMXBs) with star-formation rate (LX/SFR) change significantly with redshift, the June 2015 Outburst of V404 Cygni such that LX(LMXB)/M ~ (1+z)^2-3 and LX(HMXB)/SFR ~ In June 2015, the black hole X-ray binary (BHXRB) V404 Cygni went into outburst for the first time in 26 years. The source is not extended emission, thus, establishing Swift J1834.9-0846 as the only the closest known BHXRB, it is also known to undergo first magnetar to possess a surrounding nebula. This implies that extreme variations in brightness, allowing us to study the source’s wind nebulae are no longer exclusive to RPPs and, along with behaviour during flaring with the unprecedented detail afforded by recent discoveries in the field, further narrow the gaps between modern space and ground-based instrumentation. these two sub-populations of isolated NSs. The physical properties Here we present a timing study and a comprehensive search for of this wind nebula, however, show peculiarities, especially its high quasi-periodic oscillations (QPOs) of V404 Cygni during its most radiative efficiency of about 10%, only shared with two other recent outburst, utilizing data from six instruments on board five known very young RPPs, the Crab and its twin. different X-ray missions: Swift/XRT, Fermi/GBM, Chandra/ACIS, INTEGRAL’s IBIS/ISGRI and JEM-X, and NuSTAR. Author(s): George A. Younes2, Chryssa Kouveliotou2 , Oleg We find four previously unobserved, significant QPOs throughout Kargaltsev25 , Ramandeep Gill , Jonathan Granot 510 , Anna Watts , the outburst. One QPO, at 18 mHz, is detected in simultaneous Joseph Gelfand473 , Matthew G. Baring , Alice Kust Harding , observations with both Fermi/GBM and Swift/XRT, and is a likely George G. Pavlov62 , Alexander van der Horst , Daniela example of a rare, recently discovered class of mHz-QPOs in Huppenkothen4819 , Ersin Gögüs , Lin Lin , Oliver Roberts BHXRBs linked to high-inclination sources. We also find a broad Institution(s): 1. Beijing Normal University, 2. George structure in averaged periodograms of several Chandra/ACIS and Washington University, 3. GSFC, 4. New York University, 5. Open INTEGRAL/JEM-X observations that contains significant University, 6. Pennsylvania State University, 7. Rice University, 8. variability, but is too broad to be called a QPO, reminiscent of a Sabanci University, 9. University College Dublin, 10. University of feature more commonly observed in Cygnus X-1. We discuss our Amsterdam results in the context of current models for QPO formation. 105.05 – Constraining the State of Ultra-dense Matter Author(s): Daniela Huppenkothen1 with the Neutron Star Interior Composition Explorer Institution(s): 1. New York University [This presentation is submitted on behalf of the entire NICER Science Team] The state of cold matter at densities exceeding those 105.03 – A Repeating Fast Radio Burst: Radio and of atomic nuclei remains one of the principal outstanding problems X-ray Follow-up Observations of FRB 121102 in modern physics. Neutron stars provide the only known setting in A new phenomenon has emerged in high-energy astronomy in the the universe where these physical conditions can be explored. past few years: the Fast Radio Burst. Fast Radio Bursts (FRBs) are Thermal X-ray radiation from the physical surface of a neutron star millisecond-duration radio bursts whose dispersion measures can serve as a powerful tool for probing the poorly understood imply that they originate from far outside of the Galaxy. Their behavior of the matter in the dense stellar interior. For instance, origin is as yet unknown; their durations and energetics imply that realistic modeling of the thermal X-ray modulations observed from they involve compact objects, such as neutron stars or black holes. rotation-powered millisecond pulsars can produce stringent Due to their extreme luminosities implied by their distances and constraints on the neutron star mass-radius relation, and by the previous absence of any repeat burst in follow-up observations, extension the state of supra-nuclear matter. I will describe the many potential explanations involve one-time cataclysmic events. prospects for precision neutron star equation of state constraints However, in our Arecibo telescope follow-up observations of FRB with millisecond pulsars using the forthcoming Neutron Star 121102 (discovered in the PALFA survey; Spitler et al. 2014), we Interior Composition Explorer (NICER) X-ray timing mission. find additional bursts at the same location and dispersion measure as the original burst. We also present the results of Swift and Author(s): Slavko Bogdanov1 Chandra X-ray observations of the field. This result shows that, for Institution(s): 1. Columbia University at least a sub-set of the FRB population, the source can repeat and thus cannot be explained by a cataclysmic origin. 105.06 – X-ray Pulsation Searches with NICER The Neutron Star Interior Composition Explorer (NICER) is an Author(s): Paul Scholz8, Laura Spitler72 , Jason Hessels , X-ray telescope with capabilities optimized for the study of the Slavko Bogdanov34 , Adam Brazier , Fernando Camilo 3 , Shami structure, dynamics, and energetics of neutron stars through Chatterjee44 , James M. Cordes , Fronefield Crawford 5 , Julia S. high-precision timing of rotation- and accretion-powered pulsars in Deneva9878 , Robert Ferdman , Paulo Freire , Victoria M. Kaspi , the 0.2–12 keV band. It has large collecting area (twice that of the Patrick Lazarus7118 , Ryan Lynch , Erik Madsen , Maura XMM-Newton EPIC-pn camera), CCD-quality spectral resolution, McLaughlin13 , Chitrang Patel 8 , Scott M. Ransom 10 , Andrew and high-precision photon time tagging referenced to UTC through Seymour1126 , Ingrid H. Stairs , Benjamin Stappers , Joeri van an onboard GPS receiver. NICER will begin its 18-month prime Leeuwen27 , Weiwei Zhu mission as an attached payload on the International Space Station Institution(s): 1. Arecibo Observatory, 2. ASTRON, 3. Columbia around the end of 2016. I will describe the science planning for the University, 4. Cornell University, 5. Franklin and Marshall pulsation search science working group, which is charged with College, 6. Jodrell Bank Centre for Astrophysics, 7. Max-Planck- searching for pulsations and studying flux modulation properties of Institut fur Radioastronomie, 8. McGill University, 9. Naval pulsars and other neutron stars. A primary goal of our observations Research Laboratory, 10. NRAO, 11. NRAO, 12. University of is to detect pulsations from new millisecond pulsars that will British Columbia, 13. West Virginia University contribute to NICER’s studies of the neutron star equation of state through pulse profile modeling. Beyond that, our working group 105.04 – Unexpected Windy Weather Around a Highly will search for pulsations in a range of source categories, including Magnetized Neutron Star LMXBs, new X-ray transients that might be accreting millisecond Magnetars and rotation-powered pulsars (RPPs) historically pulsars, X-ray counterparts to unassociated Fermi LAT sources, represented two distinct subclasses of neutron stars. Magnetars are gamma-ray binaries, isolated neutron stars, and ultra-luminous slowly-rotating (~2-12 s), isolated neutron stars (NSs) with super- X-ray sources. I will survey our science plans and give an overview strong magnetic fields, B~10^13-10^15 G. RPPs, on the other of our planned observations during NICER’s prime mission. hand, are rapidly-rotating (~0.01-0.3~s), isolated NSs with surface dipole magnetic field in the range ~10^11-10^13 G. Most pulsars Author(s): Paul S. Ray2, Zaven Arzoumanian1 possess a large rotational energy loss rate that powers a relativistic Institution(s): 1. GSFC, 2. NRL magnetized particle wind, often seen as a pulsar wind nebula (PWN; the Crab PWN being the most famous). There has not yet been convincing evidence for a wind nebula around magnetars, 106 – AGNs Poster Session most likely due to their low rotational energy loss rate. Here, we report the study of new deep X-ray observations of the peculiar 106.01 – Rapid Gamma-Ray and Optical Variability in extended emission around the magnetar Swift J1834.9-0846. Our Bright Fermi Blazars new results strongly support a wind nebula as the nature of the Using an "aperture photometry" technique to generate Fermi lightcurves on minute timescales, we have searched the brightest be characteristic of the presence of relativistic jets oriented near the blazar flares for variability down to ~10 minute timescales. We find line-of-sight to the observer. As a result, we report the evidence for strong gamma-ray variability down to ~1 - 2 hour identification a number of newly discovered gamma-ray loud timescales, but not on ~10-30 minute timescales even though the NLSy1 galaxies found in the Fermi database. photon statistics are sufficient to detect it. Using SMARTS optical/NIR, we then search for correlated rapid optical variability Author(s): Hugh R. Miller1, Joseph R. Eggen1 , Jeremy on similar timescales. While variability on these very short Maune1 timescales is detected in a few cases, the optical variability Institution(s): 1. Georgia State Univ. amplitude is typically much smaller than the gamma-ray one. Interestingly, on ~1-3 daytimescales the optical and gamma-ray 106.05 – KSwAGS: A Swift X-Ray and UV Survey of the variability are instead well-correlated and of similar amplitude. We Kepler and K2 Fields discuss the implications of this variability behavior for blazar We present the first phase of the Kepler-Swift Active Galaxies and modeling. Stars survey (KSwAGS), a simultaneous X-ray and UV survey of 6 3 21square degrees of the Kepler field. Kepler/K2 is the most precise Author(s): Paolo S. Coppi , Shinya Saitoh , Lukasz Stawarz photometer of our time, producing exquisite light curves of both Institution(s): 1. Jagellonian University, 2. Rikkyo University, 3. stellar targets and active galaxies. We detect 93 unique X-ray Yale Univ. sources with signal-to-noise ratio > 3 with the XRT, of which 60 have UV counterparts. The survey produces a mixture of stellar 106.02 – Imaging AGN Feedback in NGC 3393 with sources, extragalactic sources, and sources which we are not able to CHEERS classify with certainty. We have obtained optical spectra for a The CHandra Extended Emission-line Region Survey (CHEERS) is majority of these targets, providing necessary parameters for study the 'ultimate' resolution X-ray imaging survey of nearby far-IR of the light curves in an astrophysical context; for example, surface selected AGN. By comparing deep Chandra observations with gravities and rotation velocities for stars, and black hole mass complementary HST and radio data, we investigate the morphology estimates for AGN. Our survey provides the first X-ray and UV data of the extended narrow-line region on scales of <100 pc. We for a number of known variable stellar sources, as well as a large present new results on the gas surrounding the compton-thick number of new X-ray detections in this well-studied portion of the AGN NGC 3393. The luminous extended narrow-line X-ray sky. The KSwAGS survey is currently ongoing in the K2 ecliptic emission from this gas allows us to study the role and extent of plane fields, and provides a wide array of X-ray selected targets for AGN feedback as sub-kpc jets interact with the surrounding ISM. photometric study with archival Kepler light curves and new data from K2. Author(s): Alessandro Paggi1, W. Peter Maksym1 , Giuseppina Fabbiano11 , Martin Elvis , Margarita Karovska 1 , Junfeng Wang 3 , Author(s): Krista Lynne Smith5, Patricia T. Boyd3 , Richard Thaisa Storchi-Bergmann2 Mushotzky53 , Neil Gehrels , Steve B. Howell 2 , Rick Edelson 5 , Institution(s): 1. Smithsonian Astrophysical Observatory, 2. Dawn M. Gelino14 , Alexander Brown Universidade Federal do Rio Grande do Sul, 3. Xiamen University Institution(s): 1. Caltech, 2. NASA Ames, 3. NASA GSFC, 4. University of Colorado, 5. University of Maryland College Park 106.03 – Exploring the Variability Characteristics of the Fermi AGN Sample 106.06 – Determining the X-ray Emission Mechanism The Fermi Gamma-Ray Space Telescope (Fermi) has cataloged for the Large-Scale Quasar Jet of 3C 111 over 3000 gamma-ray (>100 MeV) point sources of which ~70% Relativistic jets from active galactic nuclei (AGN) are powerful are likely AGN. The AGN are predominantly representative of the phenomena that transport prodigious amounts of energy and mass radio-loud “blazar” subclass. The emission from these objects is from the core of a galaxy out to kiloparsec or even megaparsec known to be dominated by relativistic beaming and is almost distances. While most spatially-resolved jets are seen in the radio, always variable, often exhibiting high-amplitude flaring. To date an increasing number have been discovered to emit in the there have been numerous studies of individual objects including optical/near-IR and/or X-ray bands. Here we discuss a spectacular multi-wavelength campaigns with some including parsec-scale example of this class, the 3C 111 jet, housed in one of the nearest, radio jet morphological studies. These studies have led to new double-lobed FR II radio galaxies known. The jet itself extends over insight in to our understanding of the blazar phenomena and jet 100 kpc on each side, making it one of the longest to be seen in the propagation. However, there remains a dearth of statistical radio, near-IR/optical and X-ray bands. Its length and straight information on the variability characteristics of the population in nature makes it ideal for studying jet physics over many aggregate. What, for example, are the distributions of flare kiloparsecs. We discuss new, deep Chandra and HST observations amplitudes, durations, temporal profiles and recurrence histories that reveal both near-IR and X-ray emission from several among the gamma-ray blazar subclasses? We present some results components of the 3C 111 jet, as well as both the approaching and of our study of a large ( ~103 ) set of gamma-ray light curves. For receding hotspots. The near-IR and X-ray emission in the jet is the brightest subset we explore in greater detail their properties restricted to several knots, and there are important differences such as morphologies and their rise and decay timescales. We between the morphologies seen in the radio, near-IR, and X-ray include where plausible the associated energy dependencies of bands. In several jet regions we detect X-ray maxima significantly these rise and decay profiles. We discuss our results in terms of the upstream of the radio maxima. We analyze the broad-band spectral possible implications on the scale and location of jet structures energy distributions of the jet components and the X-ray spectra of associated with the emission sites and the cooling timescales of the the brightest regions. We compare competing models of emission electron population producing the gamma rays. as they relate to frequency-dependent relativistic beaming. The morphological differences coupled with the X-ray spectral slopes Author(s): Chris R. Shrader1 lead us to favor the two-component synchrotron model and Institution(s): 1. NASA's GSFC disfavor the IC/CMB model.

106.04 – The Population of Gamma-Ray Loud NLSy1 Author(s): Devon Clautice1, Eric S. Perlman1 , Markos Galaxies With Blazar-Like Properties Georganopoulos74 , Matthew L. Lister , Francesco Tombesi 6 , Mihai 53 4 We report an investigation of the blazar-like properties for a subset Cara , Herman L. Marshall , Brandon Scott Hogan , Demos 2 of a sample of radio-loud NLSy1 galaxies. Using the properties of Kazanas rapid and large amplitude optical and radio variability, rapid and Institution(s): 1. Florida Institute of Technology, 2. Goddard large amplitude variations in the optical polarization and position Space Flight Center, 3. Massachusetts Institute of Technology, 4. angle, and choosing a sample that is very radio loud (R > 100), we Purdue University, 5. Space Telescope Science Institute, 6. find that that one can identify a sample of NLSy1 galaxies which University of Maryland, 7. University of Maryland Baltimore exhibit properties, such as gamma ray emission, that are thought to County 106.07 – Dramatic long-term X-ray variability in AGNs polarization angle swing of the blazar 3C279 reported by Abdo et al. Dramatic X-ray and optical variability on ∼ 10 year timescales has 2010. Our work has shown that this event requires an increase in been discovered recently in a handful of quasars, which may the nonthermal particles, a decrease in the magnetic field strength, provide important new insight into the issue of how luminous and a change in the magnetic field structure. We conclude that this AGNs are fueled. We have assembled a new sample of extremely event is likely due to a shock-initiated magnetic reconnection in an variable X-ray sources from archival Einstein and ROSAT data that emission environment with relatively strong magnetic energy. We could increase substantially the number of such objects known. have performed magnetrohydrodynamic simulations to support The sources in our sample varied in X-ray flux by at least a factor of this statement. Our simulations have found that the blazar 7–8 over a 10-year span, and most exhibited significantly larger emission region may be strongly magnetized. In this situation, variability amplitudes (10 to over 100). We present the details of polarization angle swings are likely to be correlated with strong how our sample was assembled and preliminary results regarding gamma-ray flares. the identifications, properties, and X-ray histories of the objects. Author(s): Haocheng Zhang3, Hui Li12 , Markus Boettcher Although a heterogeneous population is expected, some sources in Institution(s): 1. Los Alamos National Laboratory, 2. the sample are associated with broad-line AGNs, including a North-West University, 3. University of New Mexico radio-quiet quasar at z = 1.3 that decreased in X-ray luminosity by a factor of 40. 106.11 – Multi-wavelength polarimetry and variability Author(s): Edward C. Moran1 study of M87 jet during 2003-2008 Institution(s): 1. Wesleyan Univ. We present the multi-wavelength study of M87’s jet . We compare the radio and optical polarimetry and variability and attempt to 106.08 – The Vertical Structure of Nuclear Starburst study the spectrum of the jet in radio through X-rays wavelengths. Disks: Testing a Model of AGN Obscuration By comparing the data with previously published VLA and HST Nuclear starburst disks are Eddington-limited, radiation pressure observations, we show that the jet's morphology in total and supported disks that may be active in the nuclear environment of polarized light is changing significantly on timescales of ~1 decade. active galaxies (ULIRGS and AGNs). Earlier analytical models We are looking for the variability of different knots and changes in suggested that, under certain conditions, these disks may be their spectra using our deep, high resolution observations of the jet geometrically thick on pc-scales, and thus could be a viable source between 2003 and 2008. The observations have 2-3 times better for AGN obscuration, partcularly at z≤1, when gas factions in resolution that any similar previous study (Perlman et al. 1999) in galaxies are still significant. Here, we present early results from addition allowing us to observe variability. During this time, the numerical 2D models of nuclear starburst disks where the vertical nucleus showed month-scale variability in optical and X-rays and structure is calculated explicitly from solving the hydrostatic also flared twice in all wave- lengths including radio. The knot balance and radiative transfer equations. We quantitatively assess HST-1, located closest to the nucleus, displayed a huge flare, under which conditions the starburst disk may present substantial increasing about 100 times in brightness. The knot A and B obscuring columns for AGN observations. complex shows variations in polarization structures indicating the presence of a helical magnetic field which may be responsible for Author(s): David R. Ballantyne1, Raj Gohil1 the in-situ particle accelerations in the jet. We compare the Institution(s): 1. Georgia Institute of Technology evolution of different knots and components of the jet, when our observations overlap with the multi-wavelength monitoring 106.09 – The Intrinsic Eddington Ratio Distribution of campaigns conducted with HST and Chandra and comment on Active Galactic Nuclei in Young Galaxies from SDSS particle acceleration and main emission processes. We further use the data to investigate the observed 3-dimensional structure of the An important question in extragalactic astronomy concerns the jet and the magnetic field structure. distribution of black hole accretion rates, i.e. the Eddington ratio distribution, of active galactic nuclei (AGN). Specifically, it is matter Author(s): Sayali S Avachat1, Eric S. Perlman14 , Mihai Cara , of debate whether AGN follow a broad distribution in accretion Frazer N. Owen32 , Daniel E Harris , William B. Sparks 4 , kunyang rates, or if the distribution is more strongly peaked at characteristic Li11 , Katie Kosak , Markos Georganopoulos 5 Eddington ratios. Using a sample of galaxies from SDSS DR7, we Institution(s): 1. Florida Institute of Technology, 2. Harvard test whether an intrinsic Eddington ratio distribution that takes the Smithsonian Center for Astrophysics, 3. National Radio form of a broad Schechter function is in fact consistent with Astronomy Observatory, 4. Space Telescope Science Institute, 5. previous work that suggests instead that young galaxies in optical University of Maryland surveys have a more strongly peaked lognormal Eddington ratio distribution. Furthermore, we present an improved method for 106.12 – Revealing the Evolving Accretion Disk extracting the AGN distribution using BPT diagnostics that allows Corona in AGNs with Multi-Epoch X-ray us to probe over one order of magnitude lower in Eddington ratio, Spectroscopy: the case of Mrk 335 counteracting the effects of dilution by star formation. We conclude that the intrinsic Eddington ratio distribution of optically Active galactic nuclei host an accretion disk with an X-ray selected AGN is consistent with a power law with an exponential producing corona around a supermassive black hole. In bright cutoff, as is observed in the X-rays. This work was supported in sources, such as the Seyfert 1 galaxy Mrk 335, reflection of the part by a NASA Jenkins Fellowship. coronal emission off the accretion disk has been observed. Reflection produces numerous spectral features, such as the Fe Kα Author(s): Mackenzie L. Jones1, Ryan C. Hickox1 , Christine emission line and absorption edge, which allow various properties Black111 , Kevin Nicholas Hainline , Michael A. DiPompeo of the inner accretion disk and corona to be constrained. We Institution(s): 1. Dartmouth College perform a multi-epoch spectral analysis of a dozen XMM-Newton, Suzaku, and NuSTAR observations of Mrk 335, and optimize the 106.10 – MHD-based modeling of radiation and fitting procedure to unveil correlations between the Eddington polarization signatures of blazar emission ratio and multiple spectral parameters. We find that the ionization parameter of the accretion disk correlates strongly with the Observations have shown that sometimes strong multiwavelength Eddington ratio: the inner disk is more strongly ionized at higher flares are accompanied by drastic polarization variations, indicating flux. Interestingly, the slope of the correlation is less steep than active participation of magnetic fields during flares. We have previously predicted. Furthermore, the cut-off of the power-law developed a 3D numerical tool set of magnetohydrodynamics, spectrum increases in energy with the Eddington ratio, whereas the Fokker-Planck particle evolution, and polarization-dependent reflection fraction exhibits a decrease. We interpret this behaviour radiation transfer codes. This allows us to study the snap-shot as geometrical changes of the corona as a function of the accretion spectra, multiwavelength light curves, and time-dependent optical rate. Below ~10% of the Eddington limit, the compact and optically polarization signatures self-consistently. We have made a thick corona is located close to the inner disk, whereas at higher simultaneous fit of a multiwavelength flare with 180 degree accretion rates the corona is likely optically thin and extends 106.15 – GeV Blazar flares several parsecs from the vertically further away from the disk surface. Compared to previous central engine. Who pays the seed photon bill? work that considered individual spectra, we find that multi-epoch In Blazars, multi-wavelength observations suggest that some GeV spectroscopy is essential for breaking degeneracies in the spectral flares take place at the location of the mm VLBI core, several pc fits and for obtaining accurate spectral parameters. Furthermore, from the black hole. This location for the GeV emission requires a we show that this method provides a powerful tool to study coronal yet un-identified source of seed photons to be Inverse Compton evolution. The rich archives of XMM-Newton, Suzaku, and scattered to GeV energies. Our model for these flares involves a fast NuSTAR provide the opportunity to extend this investigation to spine and slow sheath configuration for the relativistic jet, where include several other bright AGN, which will reveal whether the the mildly beamed sheath emission will illuminate with a large behaviour that we found is common or unique to Mrk 335. opening angle the outer regions of the Molecular Torus. The Author(s): David R. Ballantyne1, Laurens Keek1 heated clouds will then radiate and their emission will be Institution(s): 1. Georgia Institute of Technology relativistically boosted in the spine frame where it can they be up-scattered to GeV energies. We argue, through analytical work and simulations, that this can be the seed photon source that 106.13 – Constraining Properties of AGN Coronae with produces the GeV flares. NuSTAR: the Case of the Obscured Seyfert 1.9 Nucleus MCG -05-23-016 Author(s): Peter Breiding1, Markos Georganopoulos1 , Eileen Robust measurements of the high-energy cut-off in the coronal Meyer1 continuum of AGN have long been limited to a small set of the Institution(s): 1. University of Maryland, Baltimore County brightest examples and almost exclusively to unobscured nuclei. We report on a direct measurement of the cut-off energy in the 106.16 – Soft X-ray Excess from Hot GRMHD Accretion nuclear continuum of the obscured Seyfert 1.9 nucleus in AGNs MCG-05-23-016 with unprecedented precision. The high In an attempt to better understand a fundamental physics behind sensitivity of NuSTAR in the hard X-ray band allows us to clearly the so called “soft X-ray excess (SE)” often observed in many disentangle the spectral curvature of the primary continuum from Seyfert AGNs, we propose a novel model where the innermost that of the reprocessed component. Using a simple accreting plasma, most likely originating from the ISCO of a phenomenological spectral model, we measured the cut-off energy standard accretion disk around a black hole, could develop into a to be 116+/-6 keV, while more complex Comptonization models fast MHD shock under strong gravity efficiently producing provided independent constraints on the kinetic temperature of the relativistic electrons in the downstream region. These energetic electrons in the corona and its optical depth. Similar to a number of particles then Compton up-scatter incoming EUV disk photons to such measurements perfomed with NuSTAR in the past few years, characterize the SE feature in AGN spectra. In this preliminary and consistent with analyses of relatively large samples of hard calculation we find that the characteristics of the modeled SE X-ray spectra from the NuSTAR survey of nearby AGN, the optical depends only on shocked electron temperature (kTe), inner disk depth was found to be of order unity for a range of assumed simple temperature (kTin), inclination (theta) and BH spin (a). As a case geometries. This means that the data are pushing the currently study we demonstrate that the model is successful in describing the available models to the limits of their validity. In combination with observed SE in Ark120 implying that the Comptonizing the observations of spectral signatures from the innermost region downstream region is very compact (~2-3 gravitational radii) of the accretion disk, and the observed variability of the resembling the putative X-ray “hot coronae”. The best-fit analyses high-energy cut-off, these results allow us to constrain the spatial suggest that kTe varies from 60keV to 140keV depending on BH extent of the AGN corona, its inhomogeneity and physical spin all with small inclination angles (~20-40deg). conditions needed to maintain its structure. 2 22 1 1 Author(s): Keigo Fukumura , Doug Hendry , Peter Clark , Author(s): Mislav Balokovic , Fiona Harrison Francesco Tombesi31 , Masaaki Takahashi Institution(s): 1. California Institute of Technology Institution(s): 1. Aichi University of Education, 2. James Madison University, 3. NASA/GSFC 106.14 – Probing Turbulence and Acceleration at Relativistic Shocks in Blazar Jets 106.17 – Uncovering Nature’s 100 TeV Particle Acceleration at relativistic shocks is likely to be important in Accelerators in the Large-Scale Jets of Quasars various astrophysical jet sources, including blazars and other Since the first jet X-ray detections sixteen years ago the adopted radio-loud active galaxies. An important recent development for paradigm for the X-ray emission has been the IC/CMB model that blazar science is the ability of Fermi-LAT data to pin down the requires highly relativistic (Lorentz factors of 10-20), extremely power-law index of the high energy portion of emission in these powerful (sometimes super-Eddington) kpc scale jets. R I will sources, and therefore also the index of the underlying discuss recently obtained strong evidence, from two different non-thermal particle population. This paper highlights how avenues, IR to optical polarimetry for PKS 1136-135 and multiwavelength spectra including X-ray band and Fermi data can gamma-ray observations for 3C 273 and PKS 0637-752, ruling out be used to probe diffusive acceleration in relativistic, oblique, MHD the EC/CMB model. Our work constrains the jet Lorentz factors to shocks in blazar jets. The spectral index of the non-thermal particle less than ~few, and leaves as the only reasonable alternative distributions resulting from Monte Carlo simulations of shock synchrotron emission from ~100 TeV jet electrons, accelerated acceleration, and the fraction of thermal particles accelerated to hundreds of kpc away from the central engine. This refutes over a non-thermal energies, depend sensitively on the particles' mean decade of work on the jet X-ray emission mechanism and overall free path scale, and also on the mean magnetic field obliquity to the energetics and, if confirmed in more sources, it will constitute a shock normal. We investigate the radiative synchrotron/Compton paradigm shift in our understanding of powerful large scale jets and signatures of thermal and non-thermal particle distributions their role in the universe. Two important findings emerging from generated from the acceleration simulations. Important constraints our work will also discussed be: (i) the solid angle-integrated on the frequency of particle scattering and the level of field luminosity of the large scale jet is comparable to that of the jet core, turbulence are identified for the jet sources Mrk 501, AO 0235+164 contrary to the current belief that the core is the dominant jet and Bl Lacertae. Results suggest the interpretation that turbulence radiative outlet and (ii) the large scale jets are the main source of levels decline with remoteness from jet shocks, with a significant TeV photon in the universe, something potentially important, as role for non-gyroresonant diffusion. TeV photons have been suggested to heat up the intergalactic medium and reduce the number of dwarf galaxies formed. Author(s): Matthew G. Baring3, Markus Boettcher2 , Errol J Summerlin1 Institution(s): 1. NASA's Goddard Space Flight Center, 2. North-West University, 3. Rice University Author(s): Markos Georganopoulos4, Eileen Meyer4 , discovery we developed a procedure that allowed us to recognize William B. Sparks31 , Eric S. Perlman , Roeland P. Van Der Marel 3 , gamma-ray blazar candidates within the sources associated in the Jay Anderson33 , S. Tony Sohn , John A. Biretta 3 , Colin Arthur Fermi catalogs with an uncertain classification. We also built a Norman23 , Marco Chiaberge method to search for blazar-like sources as potential counterpart of Institution(s): 1. FIT, 2. Johns Hopkins University, 3. STScI, 4. the unidentified gamma-ray sources (UGSs). However, to confirm UMBC the real nature of the selected candidates, optical spectroscopy is necessary. Thus, we started an optical spectroscopic campaign to 106.18 – NuSTAR Observations of Reddened Quasars observe the selected gamma-ray blazar candidates and unveil their Reddened quasars selected from the FIRST and 2MASS surveys origin. In this work we present the state-of-art of our observational appear to be in a transitional link in the merger-induced black hole campaign that allowed us to discover previously unknown growth/galaxy evolution model. We present the NuSTAR and gamma-ray blazars and a review of the results achieved to date. XMM-Newton/Chandra observations of 2 FIRST-2MASS red Future perspectives of our observing strategy developed to ''resolve quasars, F2M 0830+3759 and F2M 1227+3214. The combination the gamma-ray sky`` having all Fermi objects associated will be of broad-band X-ray coverage and physically-motivated spectral also discussed. models allow us to characterize the X-ray obscuration in these 6 6 systems. We find that much heavier obscuration is present globally Author(s): Francesco Massaro , Nuria Alvarez Crespo , Raffaele D'Abrusco412 , Marco Landoni , Nicola Masetti , Federica than along the line-of-sight for F2M 0830+3759, and that F2M 533 3 1227+3214 may also have much higher amounts of global versus Ricci , Dan Milisavljevic , Alessandro Paggi , Howard Alan Smith line-of-sight obscuration. These results are consistent with the Institution(s): 1. INAF Brera Observatory, 2. INAF IASF paradigm that red quasars are evacuating their heavy cocoon of Bologna, 3. Smithsonian Astrophysical Observatory, 4. University dust and gas, unveiling the central nucleus while higher column Federica II of Naples, 5. University of Rome Tre, 6. University of densities of gas are present globally, playing a role in reprocessing Turin the intrinsic emission. 106.22 – Evolution of Global Relativistic Jets: Author(s): Stephanie M. LaMassa8, Angelo Ricarte15 , Eilat Collimations and Expansion with kKHI and the Glikman715114 , C. Megan Urry , Daniel Stern , Tahir Yaqoob , Weibel Instability George Lansbury41512 , Francesca M. Civano , Steven E. Boggs , W. In the study of relativistic jets one of the key open questions is their Niel Brandt9911 , Chien-Ting J. Chen , Finn Christensen , William interaction with the environment. Here, we study the initial W. Craig621 , Charles James Hailey , Fiona Harrison , Ryan C. evolution of both electron-proton (e-+ - p ) and electron-positron Hickox351013 , Michael Koss , Claudio Ricci , Ezequiel Treister , (e± ) relativistic jets, focusing on their lateral interaction with William Zhang8 ambient plasma. We follow the evolution of toroidal magnetic Institution(s): 1. Caltech, 2. Columbia University, 3. Dartmouth fields generated by both the kinetic Kelvin-Helmholtz (kKH) and College, 4. Durham University, 5. ETH Zurich, 6. Lawrence Mushroom instabilities (MI). For an e-+ - p jet, the induced Livermore National Lab, 7. Middlebury College, 8. NASA GSFC, 9. magnetic field collimates the jet and electrons are perpendicularly Penn State, 10. Pontificia Universidad Catolica de Chile, 11. accelerated. As the instabilities saturate and subsequently weaken, Technical University of Denmark, 12. UC Berkeley, 13. Universidad the magnetic polarity switches from clockwise to counter-clockwise de Concepcion, 14. University of Maryland Baltimore County, 15. in the middle of the jet. For an e± jet, we find strong mixing of Yale University electrons and positrons with the ambient plasma, resulting in the creation of a bow shock. The merging of current filaments 106.19 – Decoding the spectral variations in the bare generates density inhomogeneities which initiate a forward shock. Seyfert 1 galaxy Fairall 9 Strong jet-ambient plasma mixing prevents a full development of X-ray spectroscopy and variability are powerful tools to understand the jet (on the scale studied), revealing evidence for both jet the fundamental physics and accretion processes occurring in collimation and particle acceleration in the forming bow shock. active galactic nuclei. The analysis is often hampered by the wealth Differences in the magnetic field structure generated by e- - p+ and of processes occurring simultaneously, making them difficult to e± jets may contribute to the polarization properties of the disentangle. Our talk focuses on the luminous Seyfert 1 galaxy observed emission in AGN jets and gamma ray bursts. Fairall 9, whose spectrum and timing behavior is much simpler, as 8 it is not affected by absorption processes. We aim to present a Author(s): Ken-Ichi Nishikawa , Jacob Trier Trier 66 2 comprehensive spectral and timing study, based on an observing Frederiksen , Aake Nordlund , Yosuke Mizuno , Philip E. 11 4 3 10 campaign performed in 2014. It consisted of a long-term Swift Hardee , Jacek Niemiec , Jose Gomez , Asaf Pe'er , Ioana 51279 monitoring, three pointed XMM observations and one NUSTAR Dutan , Athina Meli , Helene Sol , Martin Pohl , Dieter 1 observation, performed jointly with one of XMM pointings. The Hartmann different flux states of the pointed XMM observations allow us to Institution(s): 1. Clemson University, 2. Goethe University, 3. identify the continuum as the main variability driver and constrain IAA/CSIC, 4. Institute of Nuclear Physics PAN, 5. Institute of Space the accretion disk parameters with unprecedented quality. We are Science, 6. NBI, 7. Observatore de Paris-Meudon, 8. UAH/Physics, also able to establish that the source geometry remained absolutely 9. Universitaet Potsdam, 10. University College Cork, 11. unchanged over several months, a behavior not seen in other AGN. University of Alabama, 12. University of Gent We study the connection of the UV and X-ray emission from the long-term Swift monitoring and establish that the UV lags the 106.23 – The NuSTAR View of Reflecting and X-rays by several days. These time lags are then compared, Absorbing Circumnuclear Material in AGN together with the UV rms spectrum, to what is expected for a The physical conditions and precise geometry of the accreting standard thin accretion disk and put into context of the results circumnuclear material in the vicinity of supermassive black holes from the analysis of the XMM and NuSTAR data. Taken together remain open and critical questions. Between July 2012 and this will provide us with the most complete picture of this AGN yet. February 2013, NuSTAR and XMM-Newton performed four long-look joint observations of the type 1.8 Seyfert, NGC 1365. We Author(s): Anne Lohfink1, Christopher S. Reynolds2 , William have analyzed the variable absorption seen in these observations in Alston11 , Ciro Pinto order to characterize the geometry of the absorbing material. Two Institution(s): 1. University of Cambridge, 2. University of of the observations caught NGC 1365 in an unusually low Maryland absorption state, revealing complexity in the multi-layer absorbers which had previously been hidden, including a the Compton-thick 106.20 – The Gamma-Ray Blazar Quest: state of the art torus, BLR clouds, and a patchy absorber with a variable column and future perspectives around 1022 cm -2 and a line of sight covering fraction of 0.3–0.9 In 2011 we discovered that gamma-ray blazars detected by Fermi which responds directly to the intrinsic source flux, possibly due to show extremely peculiar infrared colors. On the basis of this a wind geometry. We have also analyzed two NuSTAR observations of NGC 7582, a well-studied X-ray bright Seyfert 2 with moderately additional diagnostics on the leptonic and the hadronic models. We heavy highly variable absorption and strong reflection spectral have developed a 3D multi-zone, time-dependent hadronic model features. Changes in the spectral shape and high reflection based on Fokker-Planck equations. Coupled with a polarization- fractions have led to competing explanations: 1) the central X-ray dependent radiation transfer code 3DPol, we derive the snap-shot source partially “shut off”, decreasing in intrinsic luminosity, with a spectral energy distributions and frequency-dependent polarization delayed decrease in reflection features due to the light-crossing signatures, as well as multi-wavelength light curves and time of the Compton-thick material or 2) the source became more polarization variations. These findings can be confronted with heavily obscured, with only a portion of the power law continuum future high-energy polarization observations to distinguish leaking through. The high quality of the NuSTAR spectra above 10 between the leptonic and the hadronic models. keV give us the best look at the reflection hump to date and allow us to test these two scenarios. Author(s): Haocheng Zhang3, Chris Scott Diltz2 , Markus Boettcher1 Author(s): Elizabeth Rivers1 Institution(s): 1. North-West University, 2. Ohio University, 3. Institution(s): 1. Caltech University of New Mexico

106.24 – The Extremes of Quasar Variability 106.27 – The Extreme Gravitationally Redshifted Variability is one of the key observational properties of quasars, Fe-line constraining the Rotation of the Super- and it can be used as a probe of their fueling, physics, and Massive Black Hole in Mrk 876 evolution. A new generation of synoptic sky surveys, in Most galaxies undergo one or more eras of Active Galactic Nucleus combination with the novel data analytics tools, offers (AGN) activity throughout their existence. During this era their unprecedented data sets for the studies of quasars in the time environment, under the influence of gravity due to the central domain. I will illustrate this with examples from the Catalina super-massive black hole, emits from X-ray to soft gamma-ray Real-Time Transient Survey (CRTS), which has an open and energies. Therefore these spectra and their features carry growing archive of 500 million light curves, including 350,000 information on the extreme gravitational conditions that describe spectroscopically confirmed quasars, with the time baselines the super-massive black hole. However these spectral features can ranging from 10 minutes to 10 years. I will discuss a new approach be transient and shifted to unexpected energies making their to discover quasars using a combination of variability and mid-IR detection difficult. Consequently, properties of the super-massive colors from WISE, which results in a catalog of over a million black hole can go undetected. quasar candidates. I will then discuss quasars with extreme, We present our recent results of a case study on the AGN Mrk 876. anomolous light curves, including quasars that have gone through The detection of a transient and extreme gravitationally redshifted extreme brightening events over the past decade with concordant Fe-line feature in the X-ray spectrum allows us to find its emission large changes in their spectroscopic properties. I will also discuss a mechanism, thereby constraining the rotation of the super-massive small subset of quasars with periodic light curves which we black hole in the center of Mrk 876. This finding together with a interpret as a signature of close (milliparsec scale) supermassive morphological study of the source might give a consistent picture black hole (SMBH) binaries. on the evolution of AGN.

Author(s): Daniel Stern1 Author(s): Eugenio Bottacini1 Institution(s): 1. JPL/ Caltech Institution(s): 1. Stanford

106.25 – Swift multi-wavelength observations of the 106.28 – Interpreting Sgr A*'s Most Luminous X-ray high-redshift Blazar S5 0836+710 (4C 71.07) Flares We present the preliminary results of a year-long Swift monitoring During ambitious X-ray and radio monitoring campaigns with campaign of the high-redshift (z=2.172) flat-spectrum radio quasar Chandra, XMM, Swift, and the VLA, we have detected the (FSRQ) S5 0836+710 (4C 71.07). The campaign, based on one brightest-ever X-ray flares from Sgr A*. These flares likely probe observation per month, 5 ks each observation, for 12 months, the physical processes and accretion flow near the black hole's allowed us to investigate the synchrotron and nuclear emission event horizon. Yet, despite years of observational and theoretical contributions to the optical-UV frequency range of its spectral study, we do not have a complete, unique model to explain these energy distribution and the X-ray spectral variations along a high-energy flares, or their relationship to variability at other baseline of a year. We obtained a high-accuracy determination of wavelengths. Viable models range from the tidal disruption of UVOT magnitudes, an X-ray photon index with an uncertainty of asteroids to collimated outflows to magnetic reconnection, the order of 5%, and well-sampled light curves both in the motivating observers to place tighter constraints on the timing and optical-UV and X-ray energy bands to study their possible multiwavelength properties of these outbursts. X-ray flares may modulations and correlations. Our study allowed us to exploit the also help us relate Sgr A* to weakly accreting black holes across the unique Swift capabilities in terms of both simultaneous energy mass spectrum. I will discuss the possible origins and continuing coverage and schedule flexibility. The Swift monitoring campaign mysteries surrounding Sgr A*'s high-energy flares and give a brief was supported by observations by the GLAST-AGILE Support update on the Sgr A*/G2 interaction. Program (GASP) of the Whole Earth Blazar Telescope (WEBT) Collaboration, which provided radio, near-infrared, and optical Author(s): Daryl Haggard3, Frederick K. Baganoff4 , Daniel M. photometric data as well as optical polarimetry. Moreover, a Capellupo3447 , Joseph Neilsen , Michael Nowak , Sera Markoff , spectroscopic monitoring was obtained at the William Herschel Gabriele Ponti216 , Nathalie Degenaar , Craig O. Heinke , Farhad Telescope (WHT) and the Nordic Optical Telescope (NOT). All Yusef-Zadeh5 these observations will allow us to obtain a comprehensive picture Institution(s): 1. Cambridge University, 2. Max Planck Institute of the jet as well as of the nuclear source emission. for extraterrestrial Physics, 3. McGill University/McGill Space Institute, 4. MIT Kavli Institute, 5. Northwestern Author(s): Stefano Vercellone2, Patrizia Romano2 , Claudia University/CIERA, 6. University of Alberta, 7. University of Maria Raiteri313 , Jose Acosta Pulido , Massimo Villata , Maria Amsterdam Isabel Carnerero Martin3 Institution(s): 1. IAC, 2. INAF-IASF Palermo, 3. INAF-OATO 106.29 – Particle acceleration from an inner accretion disc into compact corona and further out: case of an 106.26 – X-ray and gamma-ray polarization signatures organised magnetic field near a supermassive black of 3D multi-zone time-dependent hadronic model of hole blazar emission Upcoming observational techniques in X-rays and millimeter The origin of the high-energy spectral component of blazar spectral bands will allow to probe the inner corona of accretion emission is still controversial. Polarization signatures can provide discs near supermassive black holes. Size of this region only a few gravitational radii has been inferred from various circumstantial leading to excess γ-ray emission which may be observable also in evidence. To populate ithe region with particles, pair-creation in off-axis viewing directions (i.e., like in radio galaxies) when ergosphere and transport of particles via accretion have been deflected by moderately strong magnetic fields. Here, we invoked. investigate the time dependence of the Compton γ-ray emission Electromagnetic fields are a likely agent of acceleration in strong from such VHE γ-ray induced pair cascades. We show that the gravity of a rotating black hole. We put forward a scenario with an cascade emission is variable on time scales much shorter than the organised component of the magnetic field near a supermassive light-crossing time across the characteristic extent of the external black hole. An emergent flow of particles may be induced in a radiation field, depending on the viewing angle and γ-ray energy. preferentially bi-polar direction. Our mechanism does not seem to Thus, we find that the cascade Compton interpretation for the be capable of producing ultra-high energy cosmic rays but it does Fermi γ-ray emission from radio galaxies is still consistent with the expel particles along unbound trajectories. day-scale variability detected in the Fermi γ-ray emission of radio The mentioned concept is relevant also from a purely theoretical galaxies, such as NGC 1275, which we use as a specific example. viewpoint of dynamical properties of particle motion in General Relativity, namely, the onset of chaos near a black hole. We Author(s): Parisa Roustazadeh2, Markus Boettcher1 , conclude that the role of black-hole spin in setting the chaos is Samantha Thrush2 more complicated than initially thought (based on http://arxiv.org Institution(s): 1. Centre for Space Research, North-West /abs/1408.2452). University, 2. Ohio University

Author(s): Vladimir Karas1, Ondrej Kopacek1 , Devaky 106.33 – Swift/BAT and MAXI/GSC broadband Kunneriath12 , Jiri Kovar , Petr Slany 2 transient monitor Institution(s): 1. Astronomical Institute, 2. Silesian University "Time-domain astronomy" is one of the frontier field of astronomy for the next decade. Since the most of the transient sources show 106.30 – PKS 1510-089: Fifteen years of X-ray the temporal variation in a broad spectral range, it would be ideal to Monitoring have the real time transient monitor which covers a wide energy The blazar PKS 1510-089 is one of the best-monitored of all band. We present the newly developed broadband transient blazars, due to near-continuous monitoring by the RXTE and monitor using the Swift Burst Alert Telescope (BAT) and the MAXI SWIFT satellites at weekly or better intervals. The RXTE data, in Gas Slit Camera (GSC) data. Our broadband transient monitor particular, provide a well-sampled (~twice per week for 10 months monitors high-energy transient sources from 2 keV to 200 keV in per year) 3-color (2-4 keV, 4-7 keV and 7-10 keV) light curve seven energy bands by combining the BAT (15–200keV) and the spanning from 1996 to 2011. SWIFT data both overlap with the GSC (2–20keV) data. Currently, daily and 90-minute (one orbit) RXTE data stream and extend it up through the present day. The averaged light curves are available for 106 high-energy transient resulting light-curve gives us an excellent tool to correlate with sources. Our broadband transient monitor is available to the public Fermi observations. Both Fermi and SWIFT have observed the through our web server, http://yoshidalab.mydns.jp source from 2008 to 2015. We will present an analysis of the light /bat_gsc_trans_mon/, for wider use by the community. We curve, including a search for orphan flares (i.e., flares observed in discuss the daily sensitivity of our monitor and possible future only a single band), one of which was detected in early 2009 in PKS improvements to our pipeline. 1510-089 by Marscher et al. (2010). Cross-correlation of multi- wavelength light curves and studies of orphan flares could provide Author(s): Takanori Sakamoto1, Ryoma Oda1 , Tatehiro insight into leptonic and hadronic blazar emission models. Mihara415 , Atsumasa Yoshida , Makoto Arimoto , Scott Douglas Barthelmy353 , Nobuyuki Kawai , Hans A. Krimm , Satoshi Author(s): Evan Smith1, Eric S. Perlman11 , Jamie Holder Nakahira24 , Motoko Serino Institution(s): 1. Florida Institute of Technology Institution(s): 1. Aoyama Gakuin University, 2. JAXA, 3. NASA/GSFC, 4. RIKEN, 5. Tokyo Institute of Technology 106.31 – A Study of the X-ray Periodicities in the Remarkable Transient Source Swift J1644+57 Swift J1644+57 was discovered when it exhibited bright X-ray 107 – Astroparticles, Cosmic Rays, and activity that was believed to be triggered from the infall of a tidally disrupted star near a massive black hole. The observation of a tidal Neutrinos Poster Session disruption event (TDE) can provide clues to the geometry and 107.01 – Observational Study on Connection between physics near the black hole. If a jet forms, as we think happened Sprites and TGFs with GRT-WF with Swift J1644+57, it can provide data to study jet creation and the density of matter in a possible accretion disc. We have analyzed Although it is known that terrestrial gamma-ray flashes (TGFs) can Swift X-ray Telescope (XRT) observations of Swift J1644+57 from be caused by the electron-cosmic ray Bremsstrahlung in the initial onset to 502 days after TDE onset. We used a Z-transform presence of the Earth magnetic field, the acceleration process of Discrete Correlation Function (ZDCF) to search for periodicities in electrons in the Earth atmosphere is not clearly understood. On the the Swift X-ray light curve. We analyzed the X-ray light curve in other hand, electrons inside thunderclouds produce lightnings five time regions, including 0 to 4.5 days after TDE onset, 4.5 to 55 (under the clouds) as well as sprites (above the clouds). We study days after TDE onset, 55 to 104 days after TDE onset, 104 to 145 the connection between sprites and TGFs since both of them days after TDE onset, and 145 to 502 days after TDE onset. After require free atmospheric electrons. We constructed Goddard implementing red and white noise reduction modeling to our ZDCF Robotic Telescope - Wide Field (GRT-WF) in June 2011, which is analysis, we found plausible detections of periodicities. We briefly composed of seven wide field optical camera located at Florida Gulf discuss implications of these periods on the geometry and feeding Coast University (FGCU), to observe sprites in all the sky. We have of the tidal disruption event. recorded about 600 sprites so far, and studied possible associations Author(s): Christopher Griffith1, Abraham Falcone2 with TGFs detected by NASA’s Fermi/GBM and RHESSI. The Institution(s): 1. Naval Research Laboratory, 2. Penn State location of GRT-WF has been chosen because the area is one of the highest TGF detection regions by Fermi/GBM (others are Africa and South-East Asia). 106.32 – Time-Dependence of VHE Gamma-Ray induced Pair Cascades in Radio Galaxies Author(s): Ken Watanabe2, Takanori Sakamoto1 , Jakob Recently, several intermediate frequency peaked BL Lac objects Hegley 22 , Joseph Schlitz , Ekaterina Vydra 2 , Takashi Okajima 3 , (IBL), low frequency peaked BL Lac objects (LBL) and flat Neil Gehrels3 spectrum radio quasars (FSRQ) were detected as very high energy ( Institution(s): 1. Aoyama Gakuin University, 2. Florida Gulf VHE, E > 100 ∼ GeV) γ-ray sources. These discoveries suggest that Coast Univ., 3. NASA's GSFC γγ absorption and pair cascades might occur in those objects, 107.02 – Cosmic rays and their modulation in the propagation models, B-fields, and foreground component heliosphere by studying gamma rays from the Sun separation analysis need to be studied simultaneously in order to with Fermi-LAT: updated models properly obtain and interpret the synchrotron foreground. Indeed for the officially released Planck maps, we use only the best spectral The Sun is a known quiescent gamma-ray source. Its gamma-ray model from our above paper for the component separation steady-state, characterized by two distinct emissions, is unique for analysis. its spatially and spectrally distinct components: 1) disc emission Here we present a collections of our latest results on synchrotron, due by pion decay of CR hadrons interacting with the solar CRs and B-fields in the context of CR propagation, showing also atmosphere; 2) spatially extended emission from inverse Compton our recent work on B-fields within the Planck Collaboration. We (IC) scattering of CR electrons on the solar photons of the underline also the importance of using the constraints on CRs that heliosphere. Being produced by CRs, which are affected by solar we obtain from gamma ray observations. Methods and perspectives modulation, the intensity of both emissions is expected to be for further studies on the synchrotron foreground will be inversely proportional to the solar activity. After the discovery of addressed. the quiet solar emission with EGRET, thanks to the high sensitivity of Fermi-LAT we can now monitor the solar steady-state in the Author(s): Elena Orlando1 various periods of solar activity. The release of Pass 8 data, with its Institution(s): 1. Stanford University improved event reconstruction and larger effective area, provides a unique opportunity to refine the study and extend it to different solar activities and also to lower and higher energies. In fact a first study was conducted using 18 month of data during low solar 108 – Cosmic Backgrounds and Deep activity, where the best model for IC emission was investigated. Surveys Poster Session Now the recent CR electron and positron measurements by Pamela, AMS-02, Fermi, and the changed solar activity call for a 108.01 – Clustering, Cosmology and a New Era of more extended analysis. We present here updates on solar IC Black Hole Demographics: The Conditional models based on available CR measurements for different solar Luminosity Function of AGNs activity. Deep X-ray surveys have provided a comprehensive and largely unbiased view of AGN evolution stretching back to z 5. However, 3 1 ∼ Author(s): Elena Orlando , Nicola Giglietto , Igor V it has been challenging to use the survey results to connect this 31 2 Moskalenko , Silvia Raino' , Andrew Strong evolution to the cosmological environment that AGNs inhabit. Institution(s): 1. INFN, 2. MPE, 3. Stanford University Exploring this connection will be crucial to understanding the triggering mechanisms of AGNs and how these processes manifest 107.03 – A multi-messenger search for the origin of in observations at all wavelengths. In anticipation of upcoming high-energy astrophysical neutrinos with VERITAS wide-field X-ray surveys that will allow quantitative analysis of and Fermi AGN environments, we present a method to observationally constrain the Conditional Luminosity Function (CLF) of AGNs at a The astrophysical flux of TeV-PeV neutrinos discovered by the specific z. Once measured, the CLF allows the calculation of the IceCube observatory is likely to originate in hadronic interactions AGN bias, mean dark matter halo mass, AGN lifetime, halo at or near cosmic-ray accelerators. While no point-sources of occupation number, and AGN correlation function – all as a neutrinos have been identified so far, it may be possible to detect function of luminosity. The CLF can be constrained using a them indirectly by searching for the emission of pion-decay gamma measurement of the X-ray luminosity function and the correlation rays produced in such interactions. The sensitivity of present length at different luminosities. The method is demonstrated at z gamma-ray instruments, such as the Fermi space telescope and the ≈0 and 0.9, and clear luminosity dependence in the AGN bias and VERITAS air Cherenkov telescope array, can be used to search for a mean halo mass is predicted at both z. The results support the idea GeV-TeV gamma-ray signature from the neutrino directions. We that there are at least two different modes of AGN triggering: one, present preliminary results from 2 years of VERITAS observations at high luminosity, that only occurs in high mass, highly biased of muon-neutrino event positions detected by IceCube and discuss haloes, and one that can occur over a wide range of halo masses current plans to implement prompt follow-up observations of these and leads to luminosities that are correlated with halo mass. This events. We also report on the analysis of Fermi-LAT data for these latter mode dominates at z<0.9. The CLFs for Type 2 and Type 1 events which enhances the sensitivity of this search to fast AGNs are also constrained at z ≈0, and we find evidence that transient sources. unobscured quasars are more likely to be found in higher mass halos than obscured quasars. Thus, the AGN unification model Author(s): Marcos Santander1 seems to fail at quasar luminosities. Institution(s): 1. Barnard College - Columbia University Author(s): David R. Ballantyne1 107.04 – Galactic synchrotron radiation from radio to Institution(s): 1. Georgia Institute of Technology microwaves, and its relation to cosmic-ray propagation models: past, present and future 108.02 – The cosmic mult-messenger background Galactic synchrotron radiation observed from radio to microwaves field is produced by cosmic-ray (CR) electrons propagating in magnetic The cosmic star formation history associated with baryon flows fields (B-fields). The low-frequency foreground component within the large scale structure of the expanding Universe has separated maps by WMAP and Planck depend on the assumed many important consequences, such as cosmic chemical- and synchrotron spectrum. The synchrotron spectrum varies for galaxy evolution. Stars and accreting compact objects subsequently different line of sights as a result of changes on the CR spectrum produce light, from the radio band to the highest photon energies, due to propagation effects and source distributions. Our present and dust within galaxies reprocesses a significant fraction of this knowledge of the CR spectrum at different locations in the Galaxy light into the IR region. The Universe creates a radiation is not sufficient to distinguish various possibilities in the modeling. background that adds to the relic field from the big bang, the CMB. As a consequence uncertainties on synchrotron emission models In addition, Cosmic Rays are created on variouys scales, and complicate the foreground component separation analysis with interact with this diffuse radiation field, and neutrinos are added as Planck and future microwave telescopes. Hence, any advancement well. A multi-messenger field is created whose evolution with in synchrotron modeling is important for separating the different redshift contains a tremendous amount of cosmological foreground components. information. We discuss several aspects of this story, emphasizing The first step towards a more comprehensive understanding of the background in the HE regime and the neutrino sector, and degeneracy and correlation among the synchrotron model disccus the use of gamma-ray sources as probes. parameters is outlined in our Strong et al. 2011 and Orlando et al. 2013 papers. In the latter the conclusion was that CR spectrum, Author(s): Dieter Hartmann1 properties is broken only by the peak frequency of the ionizing Institution(s): 1. Clemson Univ. SED, which is in the UV in AGN and in X-rays in XRBs. This difference implies that the inner regions of the XRB winds are far more ionized than those of AGN, resulting in much smaller 109 – Galactic Black Holes Poster Session velocities for the same ionic species (e.g. Fe XXV) in XRB (v~1,000 km/s) than in AGN (v~10,000 km/s), in agreement with 109.01 – Multi-wavelength Observations of Fast observation. Estimates of the wind mass flux deduced from our Infrared Flares from V404 Cygni in 2015 photonization modeling, imply that the latter is much larger than We used the fast photometry mode of our new Canarias InfraRed that needed to power the observed X-ray emission, a property that Camera Experiment (CIRCE) on the 10.4-meter Gran Telescopio appears to be generic from the Galactic to the AGN black hole mass Canarias to observe V404 Cyg, a stellar mass black hole binary, on range suggesting a common underlying structure. June 25, 2015 during its 2015 outburst. CIRCE provided 10Hz Author(s): Demosthenes Kazanas2, Keigo Fukumura1 , Chris sampling in the Ks-band (2.2 microns) In addition, we obtained 23 4 simultaneous multi wavelength data from our collaborators: three R. Shrader, Ehud Behar, Francesco Tombesi GHz radio bands from the AMI telescope and three optical/UV Institution(s): 1. JMU, 2. NASA/GSFC, 3. Technion, 4. bands (u', g', r') from ULTRACAM on the William Herschel University of Maryland 4.2-meter telescope. We identify fast (1-second) IR flares with optical counterparts of varying strength/color, which we argue arise 109.04 – No Disk Winds in Failed Black Hole from a relativistic jet outflow. These observations provide Outbursts? New Observations of H1743-322 important constraints on the emission processes and physical The rich and complex physics of stellar-mass black holes in conditions in the jet forming region in V404 Cygni. We will discuss outburst is often referred to as the "disk-jet connection," a term these results as well as their implications for relativistic jet that encapsulates the evolution of accretion disks over several formation around stellar-mass black holes. orders of magnitude in Eddington ratio; through Compton scattering, reflection, and thermal emission; as they produce steady Author(s): Stephen S. Eikenberry2, Yigit Dallilar2 , Alan compact jets, relativistic plasma ejections, and (from high spectral Garner2243 , R. Deno Stelter , Poshak Gandhi , Vik Dhillon , Stuart resolution revelations of the last 15 years) massive, ionized disk Littlefair3511 , Thomas Marsh , Rob P Fender , Kunal Mooley winds. It is well established that steady jets are associated with Institution(s): 1. Oxford University, 2. Univ. of Florida, 3. radiatively inefficient X-ray states, and that winds tend to appear University of Sheffield, 4. University of Southhampton, 5. during states with more luminous disks, but the underlying University of Warwick physical processes that govern these connections (and their changes during state transitions) are not fully understood. I will 109.02 – Reflection Spectroscopy of the Black Hole present a unique perspective on the disk-wind-jet connection Binary XTE J1752-223 in the Bright Hard State based on new Chandra HETGS, NuSTAR, and JVLA observations During its rise to maximum in 2009, XTE J1752-223 stalled for a of the black hole H1743-322. Rather than following the usual full month in the bright hard state at about 30% of its peak outburst track, the 2015 outburst of H1743 fizzled: the disk never (Eddington) luminosity. Along this extended period, 60 RXTE appeared in X-rays, and the source remained spectrally hard for the pointed observations showed the luminosity and hardness ratio of entire ~100 days. Remarkably, we find no evidence for any the source to be extraordinarily stable, resulting in a unique data accretion disk wind in our data, even though H1743-322 has set of exceptional quality. We combined all these 300 ks of RXTE produced winds at comparable hard X-ray luminosities. I will data into a single PCA (3-45 keV) spectrum with 82 million counts discuss the implications of this "failed outburst" for our picture of and a single HEXTE spectrum (20-250 keV) with 10.4 million winds from black holes and the astrophysics that governs them. counts. Using our calibration tools PCACORR and HEXBCORR, Author(s): Joseph Neilsen3, Mickael Coriat25 , Sara Motta , we greatly enhanced the sensitivity of the detectors to faint spectral 54 1 features, such as the Fe line and edge. Fitting the PCA+HEXTE Rob P Fender , Gabriele Ponti , Stephane Corbel spectrum using an advanced version of our reflection code, which Institution(s): 1. CEA Saclay, 2. IRAP, 3. MIT Kavli Institute, 4. includes a physical model of Comptonization, we constrained: the MPIE, 5. Oxford University spin of the black hole (or alternatively the inner radius of the accretion disk); the inclination of the system; the ionization state 109.05 – A Super-Eddington, Compton-Thick Wind in and Fe abundance of the disk's atmosphere; and the temperature GRO J1655-40? and optical depth of the corona. We compare these results with During its 2005 outburst, GRO J1655-40 was observed at high similar ones we reported earlier for GX 339-4 in the bright hard spectral resolution with the Chandra HETGS, revealing a spectrum state. XTE J1752-223 and GX 339-4 are the first two of 29 black rich with blueshifted absorption lines of elements ranging from hole binaries we propose to study using recalibrated RXTE archival oxygen to nickel, including exotic metals like titanium and data and our reflection models. scandium. It has been argued that magnetic fields must be responsible for the dense accretion disk wind that produces these Author(s): Javier Garcia2, James F. Steiner3 , Victoria deep absorption lines. But questions about this outburst remain, Grinberg321 , Jeffrey E. McClintock , Thomas Dauser , Ronald A. because the presence of this exotic wind coincides with extremely Remillard3 soft and curved X-ray spectra, remarkable X-ray variability, and Institution(s): 1. Dr. Karl Remies Observatory , 2. Harvard- bright, unexpected optical/infrared emission that varies on the Smithsonian Center for Astrophysics, 3. Massachusetts Institute of orbital period. I will argue that the unusual features of this Technology "hypersoft state" are natural consequences of a super-Eddington Compton-thick wind from the disk. 109.03 – Photoionization modeling of GRO 1655-40: A scaled down AGN Warm Absrobers! Author(s): Joseph Neilsen2, Farid Rahoui12 , Jeroen Homan , Michelle Buxton3 We present photoinization models of the absorption features Institution(s): 1. ESO, 2. MIT Kavli Institute, 3. Yale Galactic X-ray Binary (XRB) by implementing the MHD accretion disk wind models employed to account for the ionization properties 109.06 – X-ray spectral analysis of the steady states of of the AGN Warm Absorbers (WA)(Fukumura et a. 2010). The GRS 1915+105 implementation of the same models rests on the fact that the radial Of the black hole binaries (BHBs) discovered thus far, GRS density profiles of these winds, n(r)~1/r, guarantees the correct 1915+105 stands out as an exceptional source primarily due to its values of the hydrogen equivalent column NH of the most wild X-ray variability, the diversity of which has not been replicated important ionic species at the correct values of their ionization in any other stellar-mass black hole. Although extreme variability is parameter ξ and velocity v. The similarity of the winds' ionization commonplace in its light-curve, about half of the observations of GRS1915+105 show fairly steady X-ray intensity. We report on the extreme variability on both long and short timescales, as well as X-ray spectral behavior within these steady observations. Our work complex broadband X-ray spectra. More recently, after having is based on a vast RXTE/PCA data set obtained on GRS 1915+105 returned to quiescence, V404 Cygnus also exhibited an unexpected during the course of its entire mission and 10 years of radio data re-brightening only ~6 months later. In this talk I will present an from the Ryle Telescope, which overlap the X-ray data. We find overview of the NuSTAR campaign, and discuss some early results that the steady observations within the X-ray data set naturally from these observations. separate into two regions in a color-color diagram, which we refer to as steady-soft and steady-hard. GRS 1915+105 displays Author(s): Dom Walton2, NuSTAR Collaboration1 significant curvature in the Comptonization component within the Institution(s): 1. Caltech, 2. NASA/JPL PCA band pass suggesting significantly heating from a hot disk present in all states. A new Comptonization model 'simplcut' was 109.09 – X-ray flare properties of Sgr A* developed in order to model this curvature to best effect. A majority Daily X-ray flaring represents an enigmatic phenomenon of Sgr A* of the steady-soft observations display a roughly constant inner --- the supermassive black hole at the center of our Galaxy. We disk radius, remarkably reminiscent of canonical soft state black report results from a systematic X-ray study of this phenomenon, hole binaries. In contrast, the steady-hard observations display a based on extensive Chandra observations obtained from 1999 to growing disk truncation that is correlated to the mass accretion rate 2012, totaling about 4.5 Ms. We detect flares, using a combination through the disk, which suggests a magnetically truncated disk. A of the maximum likelihood and Markov Chain Monte Carlo comparison of X-ray model parameters to the canonical state methods, which allow for a direct accounting for the pile-up effect definitions show that almost all steady-soft observations match the in the modeling of the flare lightcurves and an optimal use of the criteria of either thermal or steep power law state, while the data, as well as the measurements of flare parameters, including thermal state observations dominate the constant radius branch. A their uncertainties. A total of 82 flares are detected. About one large portion 80 % of the steady-hard observations matches the third of them are relatively faint, which were not detected hard state criteria when the disk fraction constraint is neglected. previously. The observation-to-observation variation of the These results combine to suggest that within the complexity of this quiescent emission has an average root-mean-square of 6%-14%, source is a simpler underlying basis of states, which map to those including the Poisson statistical fluctuation of faint flares below our observed in canonical BHBs. detection limits. We find no significant long-term variation in the quiescent emission and the flare rate over the 14 years. In 1 2 Author(s): Charith Peris , Ronald A. Remillard , James F. particular, we see no evidence of changing quiescent emission and 214 4 Steiner , Saeqa Dil Vrtilek , Peggy Varniere , Jerome Rodriguez , flare rate around the pericenter passage of the S2 star around 2002. 3 Guy G Pooley We show clear evidence of a short-term clustering for the flares on Institution(s): 1. Harvard-Smithsonian Center for Astrophysics, time scale of 20-70 ks. We will also report new results on the 2. MIT, 3. University of Cambridge, 4. University of Paris spectral and lightcurve properties of the flares, as well as their fluence-duration relation after carefully accounting for the 109.07 – Modeling the thermal X-ray emission around detection incompleteness and bias. Finally, we will use these the Galactic center from colliding stellar winds results to constrain the origin and emission mechanism of the The Galactic center is a hotbed of astrophysical activity. Powering flares, which further helps to establish Sgr A* as a unique these processes is the injection of wind material from ∼30 massive laboratory to understand the astrophysics of prevailing Wolf-Rayet (WR) stars orbiting within 12” of the super-massive low-luminosity black holes in the Universe. black hole (SMBH). Hydrodynamic simulations of such colliding and accreting winds produce a complex density and temperature Author(s): Daniel Wang1, Qiang Yuan1 structure of cold wind material shocking with the ambient medium, Institution(s): 1. University of Massachusetts creating a large reservoir of hot, X-ray-emitting gas. A Chandra X-ray Visionary Program that observed the Galactic center for 3 Ms 109.10 – High Energy Emission of V404 Cygni during resolved this diffuse emission. This work computes the X-ray 2015 outburst with INTEGRAL/SPI: Spectral analysis emission from these hydrodynamic simulations of the WR winds results, issues and solutions with the aim of reproducing the Chandra observations, amid A strong outburst of the X-ray transient V404 Cygni (= exploring a variety of SMBH feedback mechanisms. The success of GS2023-338) was observed in 2015 June/July up to a level of 50 the model is the spectrum from the 2”-5” ring around the SMBH Crab in the hard X-ray domain. matches the shape of the observed spectrum very well. This We have used the INTEGRAL/SPI data to investigate the spectral naturally explains that the hot gas comes from colliding WR winds, behavior of the source between 20 and 1000 keV during its and that the winds speeds of these stars are in general well maximum of activity. We have found striking variability patterns at constrained. The model flux in this ring and over the ±6” images of all timescales. For the 20-200 keV energy band, the huge signal to 4-9keV is ∼2.2× lower than the observations, with stronger noise ratio allows us to scrutinize the source evolution on a never feedback mechanisms leading to weaker X-ray emission since more reached timescale (30 s). At higher energy, the spectral shape can hot, X-ray-emitting gas is cleared from the spherical r < 12” be determined on a timescale < 1 h. simulation volume. Possible improvements to rectify this flux However, we note that at this level of photon flux, instrument's discrepancy are increasing the mass loss rates of the WRs and/or behavior may be severely tested and that some instrumental adding more gas into the simulation, such as from the O stars and artifacts could affect the data analysis. We have performed their winds, so the adiabatic WR shocks occur closer to their stars, thorough checks to ensure a correct handling of the SPI data and thereby becoming brighter in X-rays. present how to obtain reliable spectral results on the emission of V404 Cyg. We demonstrate that, with the correct configuration, the Author(s): Christopher Michael Post Russell1, Daniel 32 hard X-ray emission, up to the MeV region, is well described by a Wang , Jorge Cuadra two component model (Comptonisation law + cutoff power law) as Institution(s): 1. NASA/GSFC, 2. Pontificia Universidad Católica observed in Cyg X-1 and for V404 Cygni itself at lower flux levels. de Chile, 3. University of Massachusetts Amherst

109.08 – NuSTAR Observations of V404 Cygnus in Author(s): Elisabeth Jourdain1, Jean-Pierre Roques1 Outburst Institution(s): 1. IRAP/CNRS The Galactic LMXB V404 Cygnus, one of the closest known black hole binary systems, went through its first major outburst in ~25 years in summer 2015. Over the course of this event, the NuSTAR 110 – Galaxies and ISM Poster Session observatory played an active role in the substantial multi- wavelength campaign initiated, performing a series of exposures 110.02 – What dominates the X-ray emission of covering a span of several weeks. These observations revealed Andromeda at E>20 keV? New constraints from NuSTAR and Swift on a very bright, hard X-ray source spectral information, we will present gas morphology, scaling Thanks to its better sensitivity and spatial resolution, NuSTAR relations and X-ray based mass profiles and address their allows us to investigate the E>10 keV properties of nearby galaxies. implications. We now know that starburst galaxies, containing very young stellar 2 2 populations, have X-ray spectra which drop quickly above 10 keV. Author(s): Dong-Woo Kim , Craig Anderson , Douglas J. Burke222 , Giuseppina Fabbiano , Antonella Fruscione , Jennifer L. We extend our investigation of hard X-ray properties to an older 222 stellar population system, the bulge of M31. The NuSTAR and Swift Lauer , Michael L. McCollough , Douglas Morgan , Amy Mossman22 , Ewan O'Sullivan , Alessandro Paggi 2 , Ginevra simultaneous observations reveal a bright hard source dominating 1 the M31 bulge above 20 keV, which is likely to be a counterpart of Trinchieri Swift J0042.6+4112 previously detected (but not classified) in the Institution(s): 1. INAF, 2. Smithsonian Astrophysical Swift BAT All-sky Hard X-ray Survey. This source had been Observatory classified as an XRB candidate in various Chandra and XMM-Newton studies; however, since it was not clear that it is the 110.05 – The Morphology of Nearby Ultraviolet Galaxy counterpart to the strong Swift J0042.6+4112 source at higher Halos energies, the previous E < 10 keV observations did not generate We have detected diffuse ultraviolet light around highly inclined much attention. The NuSTAR and Swift spectra of this source drop galaxies within 100 Mpc, and around galaxies within 25 Mpc we can quickly at harder energies as observed in sources in starburst characterize its structure. The morphology of the diffuse light often galaxies. The X-ray spectral properties of this source are very corresponds to diffuse H-alpha and X-ray emission and is found similar to those of an accreting pulsar; yet, we do not find a above the central regions of galaxies as well as above regions with pulsation in the NuSTAR data. The existing deep HST images strong star formation. In some cases, brighter regions of diffuse indicate no high mass donors at the location of this source, further ultraviolet light correspond to cold dust seen with Herschel. The suggesting that this source has an intermediate or low mass most plausible explanation is that we are seeing extragalactic companion. The most likely scenario for the nature of this source is reflection nebulae, in which case the UV light traces the dust an X-ray pulsar with an intermediate/low mass companion similar distribution and underlying star formation. The dust masses to the Galactic Her X-1 system. We will also discuss other implied by the extragalactic flux are comparable to the dust in possibilities in more detail. galaxy disks; if the dust-to-gas ratio is constant, then these galaxies expel about as much gas as they contain. Author(s): Mihoko Yukita1, Andrew Ptak3 , Thomas J. Maccarone631 , Ann E. Hornschemeier , Daniel R. Wik , Katja Author(s): Edmund J. Hodges-Kluck1, Joel N. Bregman1 , Pottschmidt35 , Vallia Antoniou , Frederick K. Baganoff 2 , Bret Julian Cafmeyer1 Lehmer75 , Andreas Zezas , Patricia T. Boyd 34 , Jamie Kennea , Kim Institution(s): 1. University of Michigan L Page8 Institution(s): 1. Johns Hopkins University, 2. MIT, 3. 110.06 – X-ray Mass Profiles from Chandra Galaxy NASA/GSFC, 4. Penn State University , 5. SAO, 6. Texas Tech Atlas University, 7. University of Arkansas, 8. University of Leicester We present preliminary results of a Chandra/XMM-Newton joint analysis on a sample of three Early Type Galaxies (ETGs, namely 110.03 – Global MHD simulations of cosmic ray driven NGC4649, NGC4636 and NGC5846). X-ray observations of the hot galactic winds ISM is used to measure the total enclosed mass assuming hydrostatic equilibrium, and compasion with mass distributions Galactic outflows play an important role in galactic evolution. obtained through optical kinematics data of globular clusters and Despite their importance, a detailed understanding of the physical planetary nebulae yields informations about disturbances in the mechanisms responsible for the driving of these winds is lacking. ISM distribution due to nuclear activity, merging history, etc. Our In an effort to gain more insight into the nature of these flows, we analysis makes use of the Chandra Galaxy Atlas (CGA) data perform global three-dimensional magneto-hydrodynamical products - exploiting the unmatched spatial resolution of the ACIS simulations of an isolated starbursting galaxy. We focus on the detectors to reveal fine ISM features and disturbances in the inner dynamical role of cosmic rays injected by supernovae, and galactic regions - and XMM-Newton data - relying on the large field specifically on the impact of the streaming and anisotropic of view of EPIC detector to extend the mass profiles to larger radii. diffusion of cosmic rays along the magnetic fields. We find that We then measured the mass profiles in various pie sectors to these microphysical effects can have a significant effect on the wind separate different gas features (e.g., discontinuity and extended launching and mass loading factors depending on the details of the tail) and compared them with GCs/PNe based mass profiles. The plasma physics. Cosmic rays stream away from the densest regions X-ray mass profiles of NGC4649 show a generally relaxed near the galactic disk along partially ordered magnetic fields and, in morphology and, in agreement with previous analysis, the the process, accelerate more tenuous gas away from the galaxy. For comparison with the optical mass profiles shows a significant cosmic ray acceleration efficiencies broadly consistent with the deviations on parsec scale likely due to non-thermal pressure observational constraints, cosmic rays are likely to have a notable linked to nuclear activity. In significantly disturbed cases impact on the wind launching. (NGC4648 and NGC5846) where we found discontinuities and extended tails, we found that the mass profiles are over-estimated Author(s): Mateusz Ruszkowski2, Hsiang-Yi Karen Yang1 , toward the compressed discontinuity and under-estimated toward Ellen Gould Zweibel3 the extended tails, similar to inflow and outflow cases. These Institution(s): 1. University of Maryland, 2. University of preliminary results are promising toward an extended analysis of Michigan, 3. University of Wisconsin the whole CGA sample in order to study the distribution of gas temperature and metal abundances in the ISM, and to investigate 110.04 – Chandra Galaxy Atals - Global Hot Gas scaling relations between ETG global quantities like ISM Properties temperature, luminosity and total mass. The hot gas in early type galaxies (ETGs) plays a crucial role in Author(s): Alessandro Paggi2, Dong-Woo Kim2 , Craig understanding their formation and evolution. As the hot gas is 22 2 often extended to the outskirts beyond the optical size, the large Anderson , Douglas J. Burke , Giuseppina Fabbiano , Antonella Fruscione22 , Jennifer L. Lauer , Michael L. McCollough 2 , Douglas scale structural features identified by Chandra (including jets, 22 2 1 cavities, cold fronts, filaments and tails) point to key evolutionary Morgan , Amy Mossman , Ewan O'Sullivan , Ginevra Trinchieri mechanisms, e.g., AGN feedback, merging history, Institution(s): 1. INAF-Osservatorio Astronomico di Brera, 2. accretion/stripping and star formation and its quenching. In our Smithsonian Astrophysical Observatory new project, the Chandra Galaxy Atlas, we systematically analyze the archival Chandra data of ~100 ETGs to study the hot ISM. 110.08 – Search for Gamma-ray Emission from Dark Using uniformly derived data products with spatially resolved Matter Annihilation in the Small Magellanic Cloud with the Fermi Large Area Telescope Author(s): Lia Corrales2, Javier Garcia13 , Joern Wilms , The Small Magellanic Cloud (SMC) is the second-largest satellite Frederick K. Baganoff2 galaxy of the Milky Way and is only 60 kpc away. As a nearby, Institution(s): 1. Harvard Center for Astrophysics, 2. MIT Kavli massive, and dense object with relatively low astrophysical Institute for Astrophysics and Space Research, 3. University of backgrounds, it is a natural target for dark matter indirect detection Erlangen-Nuremberg searches. In this analysis, we use six years of Pass 8 data from the Fermi Large Area Telescope to search for gamma-ray signals of 110.11 – The Environment of Binary Nuetron Star dark matter annihilation in the SMC. Using data-driven fits to the Mergers gamma-ray backgrounds, and a combination of cosmological In addition to detections by LIGO, binary neutron star mergers may N-body simulations and direct measurements of rotation curves to be detected via luminous interaction with surrounding interstellar estimate the SMC dark matter density profile, we found that the media. Upcoming observations including the VLASS survey may be SMC was well described by standard astrophysical sources, and no able to detect such interactions and offer constraints on the binary signal from dark matter annihilation was detected. We set neutron star merger rate. In this talk, I will present the results of conservative upper limits on the dark matter annihilation cross cosmological simulations of a cluster of galaxies followed down to section. These constraints are in agreement with stronger redshift 0. Our calculation includes star formation from which we constraints set by searches in the Large Magellanic Cloud and infer a supernova and binary neutron star production rate. Using approach the canonical thermal relic cross section at dark matter pre-existing models of neutron star binaries, we follow the masses lower than 10 GeV in the bb and ττ+ − annihilation positions of neutron star pairs in the cluster potential throughout channels. cosmic time allowing us to identify regions in which neutron stars merge. We present statistics of many Monte Carlo instances of Author(s): Regina Caputo6, Matthew Buckley4 , Pierrick nuetron star pairs and trajectories allowing us to constrain the Martin15 , Eric Charles , Alyson Brooks 4 , Alex Drlica-Wagner 2 , approximate fraction of neutron stars merging in dense gas. Our Jennifer Gaskins35 , Matthew Wood work has implications for R-process enrichment of galaxies in Institution(s): 1. CNRS, IRAP, 2. Fermi National Accelerator addition to predicting electromagnetic counterparts to gravitational Laboratory, 3. GRAPPA, 4. Rutgers, 5. SLAC National Accelerator wave detections of neutron star mergers. Laboratory, 6. University of California Santa Cruz Author(s): Brandon Wiggins1 110.09 – The Properties of Interstellar Dust From a Institution(s): 1. Brigham Young University Survey of X-ray Halos Small-angle scattering of X-rays off interstellar dust grains produce 110.12 – Investigating Metallicity Variations in X-ray halos around bright sources along absorbed lines of sight. Early-type Galaxies with Chandra While many studies have examined these halos, no systematic Some simulations of galaxy formation predict large variations in study has compared the available halo data to the large number of the metallicity of the hot X-ray emitting galaxy atmospheres, dust models that are commonly used. To address this, we have producing a higher-emission weighted metallicity than the true obtained the largest sample yet of X-ray halos from XMM-Newton mass-weighted metallicity when a spectrum is fit. Since the and Chandra and fitted them with 14 dust grain models. We have variations may be detectable in existing data, we searched for the also compared our results with the optical extinction, AV , when it is predicted variations using X-ray intensity maps from Chandra and available in the literature. Our results can be summarized as color-color analysis, which can constrain the metallicity of an follows. (1) Comparing AVH with N values measured by X-ray isothermal plasma. Applying this analysis to 5 early-type galaxies spectral fitting, we find a ratio of AVH /N (1021 cm−2 ) = 0.48 ± revealed variations in the surface brightness distribution but these 0.06, similar to what has been found by previous workers. (2) Out variations are not simply due to changes in metallicity. NGC 5846 of 35 halos, 27 could be fit by one or more grain models, with the provides an important case study as the intensity of photons is high most successful models having maximum grain radius amax < 0.4 enough to fit spectra to small regions of the galaxy, providing a μm and fewer large grains than the less successful models. This comparison to the results of the color-color analysis. Although the suggests that the diffuse ISM does not contain a signicant presence spectra of small regions in NGC 5846 are consistent with two of grains with amax > 0.5 μm. (3) Most halos were best fit temperature (2T) models, further analysis indicates that the assuming a single dust cloud dominated the scattering, as opposed metallicities and temperatures of the 2T models must fall within a to smoothly distributed dust along the sight line. (4) Eight sources certain range of the isothermal values predicted from color-color could not be fit with the models considered here; these tended to analysis. The contribution of undetected X-ray binaries to the be distant (d > 5 kpc) sight lines through the Galactic thin disk. 5) diffuse X-rays were investigated, but they are likely not the cause of Some sight lines had halos with observed X-ray scattering optical the variations. depth τsca/A V that were significantly different than expected, which may be indicative of an inhomogeneous dust distribution Author(s): Patrick Dahlin1, Edmund J. Hodges-Kluck1 , Joel across the halo extraction area on the sky. N. Bregman1 Institution(s): 1. University of Michigan - Ann Arbor Author(s): Lynne A. Valencic1, Randall K. Smith2 Institution(s): 1. Johns Hopkins Univ., 2. SAO 110.13 – Chandra Detection of X-ray Emission from Ultra-compact Dwarf Galaxies and Extended Star 110.10 – The effects of dust scattering on Clusters high-resolution X-ray absorption edge structure We have conducted a systematic study of X-ray emission from In high resolution X-ray spectroscopy, dust scattering significantly ultra-compact dwarf (UCD) galaxies and extended star clusters enhances the total extinction optical depth and alters the shape of (ESCs), based on archival Chandra observa- tions. Among a sample photoelectric absorption edges. This effect is modulated by the dust of 511 UCDs and ESCs complied from the literature, 17 X-ray grain size distribution, spatial location along the line of sight, and counterparts with 0.5-8 keV luminosities above ∼5 × 1036 erg s−1 the imaging resolution of the X-ray telescope. We focus in are identified, which are distributed in eight early-type host particular on the Fe L-edge at 0.7 keV, fitting a template for the galaxies. To facilitate comparison, we also identify X-ray total extinction to the high resolution spectrum of three X-ray counterparts of 360 globular clusters (GCs) distributed in four of binaries from the Chandra archive: GX 9+9, XTE J1817-330, and the eight galaxies. The X-ray properties of the UCDs and ESCs are Cyg X-1. In cases where dust is intrinsic to the source, a covering found to be broadly similar to those of the GCs. The incidence rate factor based on the angular extent of the dusty material must be of X-ray-detected UCDs and ESCs, (3.3±0.8)%, while lower than applied to the extinction curve, regardless of imaging resolution. that of the X-ray-detected GCs [(7.0±0.4)%], is substan- tially We discuss the various astrophysical cases in which scattering higher than expected from the field populations of external effects need to be taken into account. galaxies. A stacking analysis of the individually undetected UCDs/ESCs further reveals significant X-ray signals, which corresponds to an equivalent 0.5-8 keV luminosity of ∼4 × 1035 70 Myr after the shocks started to develop. Therefore, the system is erg s−1 per source. Taken together, these provide strong evidence indeed in a very early phase of its collision process. that the X-ray emission from UCDs and ESCs is dominated by low-mass X-ray binaries having formed from stellar dynamical Author(s): Yuichi Kato6, Kazuhiro Nakazawa6 , Takuya interactions, consistent with the stellar populations in these dense Akahori25 , Liyi Gu , Motokazu Takizawa 7 , Yutaka Fujita 3 , Kazuo systems being predominantly old. Makishima41 , Aurora Simionescu Institution(s): 1. Institute of Space and Astronautical Science, 2. Author(s): Meicun Hou1, Zhiyuan Li1 Kagoshima University, 3. Osaka University, 4. RIKEN, 5. SRON Institution(s): 1. Nanjing University Netherlands Institute for Space Research, 6. University of Tokyo, 7. Yamagata University 110.14 – Where in the Milky Way is the North Polar Spur? 111.04 – The Merger Dynamics of Abell 2061 A series of pointed observations with XMM-Newton of the X-ray Abell 2061, a galaxy cluster at a redshift of z=.0784 in the Corona bright "North Polar Spur” (*) near l=30° and b=8° have been Borealis Supercluster, displays features in both the X-ray and radio analyzed in combination with dedicated ground-based absorption indicative of merger activity. Observations by the GBT and the measurements and three-dimensional reddening maps. There is Westerbork Northern Sky Survey (WENSS) have indicated the compelling evidence that the southern terminus of the North Spur presence of an extended, central radio halo/relic coincident with is absorption bounded and that the X-ray emitting region is behind the cluster's main X-ray emission and a bright radio relic to the SW the Aquila Rift clouds, at least hundreds of parsecs away. of the center of the cluster. Previous observations by ROSAT, Moreover, absorbing columns deduced from X-ray spectral fitting Beppo-SAX, and Chandra show an elongated structure (referred to correlate more tightly with dust optical depths from Planck than as the ‘Plume’), emitting in the soft X-ray and stretching to the NE with any other ISM column indicator, suggesting that the emission of the cluster’s center. The Beppo-SAX and Chandra observations may originate several kpc away. This result raises the question of a also suggest the presence of a hard X-ray shock slightly NE of the possible link between the Spur and outflows from the inner Galaxy cluster’s center. Here we present the details of an August 2013 (Fermi bubbles, Galactic wind). XMM-Newton observation of A2061 which has greater field of view (* Prop: 074189, P.I. K.D. Kuntz) and longer exposure (48.6 ks) than the previous Chandra observation. We present images displaying the cluster’s soft and Author(s): Rosine Lallement1, Steven L. Snowden5 , Kip hard X-ray emission and also a temperature map of the cluster. KUNTZ243 , Dimitra Koutroumpa , Isabelle Grenier , Jean-Marc This temperature map highlights the presence of a previously Casandjian3 unseen cool region of the cluster which we hypothesize to be the Institution(s): 1. CNRS, 2. Henry A. Rowland Department of cool core of one of the subclusters involved in this merger. We also Physics & Astronomy, 3. Laboratoire AIM, Université Paris discuss the structural similarity of this cluster with a simulated Diderot & CEA Saclay Irfu, 4. LATMOS/IPSL, 5. NASA/Goddard high mass-ratio offset cluster merger taken from the Simulation Space Flight Center Library of Astrophysical cluster Mergers (SLAM). This simulation would suggest that the Plume is gas from the cool core of a subcluster which is now falling back into the center of the cluster 111 – Galaxy Clusters Poster Session after initial core passage. 111.03 – Observation of a nearby early merging cluster Author(s): Avery Bailey8, Craig L. Sarazin84 , Tracy E. Clarke , of galaxies, CIZA J1358.9-4750: new born shocks in the Marios Chatzikos61 , Taylor Hogge , Daniel R. Wik 2 , Lawrence ICM Rudnick77 , Damon Farnsworth , Reinout J. Van Weeren 3 , Shea Brown5 Cluster merger events drive shocks in the intra-cluster plasma and Institution(s): 1. Boston University, 2. Goddard Space Flight activate non-thermal phenomena such as particle acceleration, Center, 3. Harvard-Smithsonian CfA, 4. Naval Research Lab, 5. magnetic field amplification, and turbulence. However, details of University of Iowa, 6. University of Kentucky, 7. University of these processes are not well known because of a lack of Minnesota, 8. University of Virginia observations. The known examples of merging clusters are mostly in late merger phases, wherein the shocks have already reached the low-density outer regions. Therefore, finding nearby merging 111.06 – Early Results from Swift AGN and Cluster clusters in early phases, in which the shock is still located in dense Survey regions, is of great importance. The Swift AGN and Cluster Survey (SACS) uses 125 deg^2 of Swift In order to find suitable objects, we searched the CIZA catalog, X-ray Telescope serendipitous fields with variable depths which collects X-ray detected cluster candidates located behind the surrounding gamma-ray bursts to provide a medium depth (4 × Zone of Avoidance, near the Galactic ridge. We found a very 10^-15 erg cm^-2 s^-1) and area survey filling the gap between promising merging-cluster candidate CIZA J1358.9-4750, with a deep, narrow Chandra/XMM-Newton surveys and wide, shallow redshift of 0.07. It consists of a close pair of X-ray clusters of ROSAT surveys. Here, we present the first two papers in a series of galaxies in North-west(NW) and South-east(SE), which are publications for SACS. In the first paper, we introduce our method connected by an X-ray bright ``bridge’’ region in between. We and catalog of 22,563 point sources and 442 extended sources. observed this object with Suzaku and Chandra, and analyzed its SACS provides excellent constraints on the AGN and cluster archival short exposure XMM-Newton data. The Suzaku data number counts at the bright end with negligible uncertainties due revealed that the NW and SE clusters have temperatures of 5.2±0.2 to cosmic variance, and these constraints are consistent with keV and 4.6±0.2 keV, respectively. The bridge region was found to previous measurements. The depth and areal coverage of SACS is have a 1.6 times higher temperature, 9.2±1.5 keV. In the existing well suited for galaxy cluster surveys outside the local universe, XMM-Newton data, we found an abrupt brightness jump reaching z > 1 for massive clusters. In the second paper, we use coinciding in position with the Suzaku high-temperature region. SDSS DR8 data to study the 203 extended SACS sources that are With additional Chandra data, we found a bright plateau with a located within the SDSS footprint. We search for galaxy width of 2’, i.e. 170 kpc. The front and back jumps are presumably over-densities in 3-D space using SDSS galaxies and their the forward and reverse shocks between the two clusters. photometric redshifts near the Swift galaxy cluster candidates. We Therefore, the object is likely to be a rather symmetric shock find 103 Swift clusters with a > 3σ over-density. The remaining system, in which two clusters of similar masses are colliding. The targets are potentially located at higher redshifts and require Mach number of the collision was derived as 1.3±0.2 and 1.17±0.04 deeper optical follow-up observations for confirmations as galaxy from the Suzaku temperature jump and the Chandra brightness clusters. We present a series of cluster properties including the jump, respectively. This Mach number and the X-ray temperature redshift, BCG magnitude, BCG-to-X-ray center offset, optical give the shock velocity as 1200 km/s. It can be combined with the richness, X-ray luminosity and red sequences. We compare the separation of the two shocks(120 kpc), to yield an age estimate of observed redshift distribution of the sample with a theoretical model, and find that our sample is complete for z ≤ 0.3 and 80% driven by AGN jets in dynamical galaxy clusters. These jets lift gas complete for z ≤ 0.4, consistent with the survey depth of SDSS. out of the center of the cluster, redistributing metals and adding These analysis results suggest that our Swift cluster selection energy to the ICM. We compare our results to X-ray observations algorithm presented in our first paper has yielded a statistically of metallicity in clusters. well-defined cluster sample for further studying cluster evolution and cosmology. In the end, we will discuss our ongoing optical Author(s): Brian J. Morsony2, Sebastian Heinz1 , Christopher identification of z>0.5 cluster sample, using MDM, KPNO, CTIO, S. Reynolds2 and Magellan data, and discuss SACS as a pilot for eROSITA deep Institution(s): 1. Univ. Of Wisconsin Madison, 2. University of surveys. Maryland

Author(s): Xinyu Dai2, Rhiannon Griffin22 , Jenna Nugent , 111.10 – A Fossil Group in Formation Christopher S. Kochanek13 , Joel N. Bregman In the current picture of hierarchical structure formation, galaxy Institution(s): 1. Ohio State univerisy, 2. Univ. of Oklahoma, 3. groups play a vital role as the seeds from which large assemblies of University of Michigan matter form. Compact groups are also important environments in which to watch the fueling of star formation and AGN activity, as 111.07 – The Role of Outburst Shock Heating in AGN the conditions are ideal for galaxy-galaxy interactions. We have Feedback identified a galaxy system that may represent an intermediate or One of the major discoveries of modern X-ray observatories is that transition stage in group evolution. Shakhbazyan 1 (or SHK 1) is a central AGN in galaxies, groups, and clusters can regulate cooling remarkably compact collection of about ten massive, red-sequence in the diffuse X-ray emitting gas. This connection is demonstrated galaxies within a region 100 kpc across. Several of these galaxies by the presence of large cavities in the diffuse gas, usually filled show signs of AGN activity, and new, deep optical observations with radio-emitting plasma, that have been evacuated by jets from with the Discovery Channel Telescope reveal an extended stellar the AGN. This AGN feedback has important consequences for star envelope surrounding the galaxies. This envelope is much more formation, galaxy evolution, super-massive black hole growth, extended than what would be expected from a superposition of galaxy/black hole scaling relations, cluster scaling relations, and normal galaxy envelopes, and it indicates a large amount of the growth of structure. Although it has generally been found that intra-group starlight, evidence that the galaxies in SHK 1 are the kinetic output of central AGN scales with the gas cooling rate dynamically interacting. and is energetic enough to offset cooling, the details of how and where this energy is transferred to heat the gas are poorly We here present new Chandra spectral imaging observations of this understood. I will discuss the role of weak AGN outburst shocks in unusual system that confirm the presence of an X-ray-emitting heating the diffuse gas, and present some results from a very deep diffuse intra-group medium (IGM), with a temperature of 1.5 keV (650 ks) Chandra observation of the galaxy group NGC 5813. With and X-ray luminosity of 1043 erg/s. Assuming hydrostatic three three pairs of collinear cavities, each pair associated with an equilibrium, the system is about 1/3 as massive as expected from elliptical AGN outburst shock, NGC 5813 is uniquely well-suited to the optical richness. In addition, three of the ten central galaxies studying the outburst history of the AGN and the mean shock exhibit signatures of X-ray AGN. The under-luminous IGM, high heating rate. density of bright galaxies, and evidence for galaxy-galaxy interaction indicate that this system may be in a transition stage of Author(s): Scott W. Randall1, Paul Nulsen11 , Christine Jones , galaxy merging, similar to that expected in the formation of a fossil William R. Forman1 group. Alternatively, SHK 1 may consist of multiple poor groups in Institution(s): 1. Harvard-Smithsonian Center for Astrophysics the final stages of merging along our line of sight. We explore these scenarios and outline paths of future study for this enigmatic 111.08 – The AGN-driven shock in NGC 4472 system. Chandra observations of most cool core clusters of galaxies have Author(s): Eric D. Miller1, Saul A. Rappaport1 , Michael revealed large cavities where the inflation of the jet-driven radio 11 1 bubbles displace the cluster gas. In a few cases, outburst shocks, McDonald , Mark W. Bautz , Catherine E. Grant , Sylvain 1 likely driven by cavity inflation, are detected in the ambient gas. Veilleux AGN-driven shocks may be key to balancing the radiative losses as Institution(s): 1. MIT shocks will increase the entropy of, and thereby heat, the diffuse gas. We will present initial results on deep Chandra observations of the nearby (D=17 Mpc) early-type massive elliptical galaxy NGC 112 – Gamma-Ray Bursts Poster Session 4472, the most optically luminous galaxy in the local Universe, lying on the outskirts of the Virgo cluster. The X-ray observations 112.01 – The statistics of BAT-to-XRT flux ratio in show clear cavities in the X-ray emission at the position of the radio GRB:Evidence for a characteristic value and its lobes, and rings of enhanced X-ray emission just beyond the lobes. implications We will present results from our analysis to determine whether the We present the statistics of the ratio, R, between the prompt and lobes are inflating supersonically or are rising buoyantly. We will afterglow ``plateau" fluxes of GRB. This we define as the ratio compare the energy and power of this AGN outburst with previous between the mean prompt energy flux inSwift BAT and the Swift powerful radio outbursts in clusters and groups to determine XRT one, immediately following the steep transition between these whether this outburst lies on the same scaling relations or whether two states and the beginning of the afterglow stage referred to as it represents a new category of outburst. the ``plateau". Like the distribution of many other GRB observables, the histogram of R is log-normal with maximum at a 3 1 Author(s): Marie-Lou Gendron-Marsolais , Ralph P. Kraft , value Rm ~ 2000, FWHM of about 2 decades and with the entire Akos Bogdan11 , William R. Forman , Julie Hlavacek-Larrondo 3 , distribution spanning about 5 decades in the value of R. We note Christine Jones11 , Paul Nulsen , Scott W. Randall 1 , Elke Roediger 2that the peak of the distribution is close to the proton-to-electron Institution(s): 1. Harvard-Smithsonian, CfA, 2. University of mass ratio R~mpe m/m=1836 , as proposed to be the case, on the Hull, 3. University of Montreal basis of a specific model of the GRB dissipation process. It therefore appears that, in addition to the values of the energy of 111.09 – Jet-driven redistribution of metal in galaxy peak luminosity Epe ~ mc2, GRB present us with one more clusters quantity with an apparent characteristic value. The fact that the The ICM in galaxy clusters is metal enriched, typically to about values of both these quantities (Ep and R ) are consistent with the 30% of solar metallicity, out to large radii. However, metals should same specific model invoked to account for the efficient conversion form mostly in galaxies and remained bound to their progenitor of their relativistic proton energies to electrons, argues favorably systems. To enrich the ICM, effective mixing of gas needs to occur for its underlying assumptions. across large scales. We carry out numerical simulations of mixing Author(s): Demosthenes Kazanas1, Judith L. Racusin1 analysis tools originally developed by the COMPTEL collaboration. Institution(s): 1. NASA/GSFC Given the nine years of COMPTEL data, we expect that this work will likely add to our understanding of the polarization properties of 112.02 – A Homogeneous Dataset for Probing the transient sources, such as GRBs and solar flares, as well as brighter Environments of Gamma-Ray Bursts steady sources, such as the Crab and Cyg X-1. Here we present Studying the spectra of long gamma-ray bursts (GRBs) is providing results from simulations of the COMPTEL polarization response greater clues about the environments in which they reside. Much and examine prospects for studying GRB polarization. of our understanding to date comes from spectral data obtained in Author(s): Mark L. McConnell2, Werner Collmar1 the gamma-ray to X-ray. Studies of the environments of individual Institution(s): 1. Max Planck Institute for Extraterrestrial bursts have additionally included UV/optical data. However, Physics, 2. Univ. of New Hampshire because of the paucity of UV/optical data in the past, the soft-energy component has not been systematically included in these studies. The Swift Ultra-Violet/Optical Telescope (UVOT) has observed more GRBs in the UV/optical than any other 113 – Gravitational Waves Poster Session telescope. From these observations we have generated a homogenous UV/optical GRB afterglow catalog. Coupling this data 113.01 – The Search for Gravitational Wave EM with archival Swift X-Ray Telescope (XRT) data, we examine the Counterparts with Swift spectral evolution of GRBs in order to probe the circumburst We present the plan to search for electromagnetic counterparts of environment. Particularly we examine the fraction of GRBs that Gravitational Waves (GWs) discovered during the current and have their cooling break between the optical and X-ray, and place upcoming runs of the LIGO and Virgo detectors. As we enter a limits on the number of bursts residing in a windy or ISM period where the sensitivity of the current generation of GW environment. detectors approaches a high probability of the first detection of a real GW signal, confirmation of the reality of these triggers will be Author(s): Peter Roming2, Jennifer Tobler31 , Stephen Holland greatly improved if an EM counterpart can be found. Swift’s ability Institution(s): 1. NASA Goggard Space Flight Center, 2. to rapidly respond to high priority target-of-opportunity Southwest Research Institute, 3. University of North Dakota observations, it’s multi-wavelength capabilities and low overhead observing make it a seemingly ideal follow-up facility. However 112.03 – Studying the high redshift Universe with comparing the size of the expected GW error regions with the fields Athena of view of the Swift XRT and UVOT telescopes, we find that Athena is the second large mission selected in the ESA Cosmic covering the large GW error regions would require a unreasonably Vision plan. With its large collecting area, high spectral-energy large number of pointings. We present our method of meeting this resolution (X-IFU instrument) and impressive grasp (WFI challenge, by both reducing the problem using Galaxy targeting, instrument), Athena will truly revolutionise X-ray astronomy. The and by operating Swift in an entirely new way in order to cover the most prodigious sources of high-energy photons are often still large number of fields needed to chase down the EM transitory in nature. Athena will provide the sensitivity and spectral counterpart before it disappears. resolution coupled with rapid response to enable the study of the Author(s): Jamie Kennea1, Phil Evans2 , Swift GW follow-up dynamic sky. Potential sources include: distant Gamma-Ray Bursts team1 to probe the reionisation epoch and find ‘missing’ baryons in the Institution(s): 1. Penn State, 2. University of Leicester cosmic web; tidal disruption events to reveal dormant supermassive and intermediate-mass black holes; and supernova explosions to understand progenitors and their environments. 113.03 – INTEGRAL upper limits on gamma-ray emission associated with the gravitational wave event Using detailed simulations, we illustrate Athena’s extraordinary GW150914 capabilities for transients out to the highest redshifts and show Using observations of the INTErnational Gamma-Ray Astrophysics how it will be able to constrain the nature of explosive transients Laboratory (INTEGRAL), we put tight upper limits on the including gas metallicity and dynamics, constraining environments gamma-ray and hard X-ray prompt emission associated with the and progenitors. gravitational wave event GW150914, discovered by the LIGO/Virgo collaboration. The omni-directional view of the Author(s): P. T. O'Brien1 INTEGRAL/SPI-ACS has allowed us to constrain the fraction of Institution(s): 1. University of Leicester energy emitted in the hard X-ray electromagnetic component for the full high-probability sky region of LIGO/Virgo trigger. Our 112.04 – GRB Polarization Measurements with upper limits on the hard X-ray fluence at the time of the event CGRO/COMPTEL range from Fγ=2x10−8 erg cm−2 to Fγ=10−6 erg cm−2 in the 75 We have embarked on a program to analyze CGRO/COMPTEL data keV - 2 MeV energy range for typical spectral models. Our results in search for evidence of polarization in both transient sources and constrain the ratio of the energy promptly released in gamma-rays in brighter steady sources. We are pursuing this work because of in the direction of the observer to the gravitational wave energy −6 the heightened interest in high energy polarimetry, the recognition Eγ /EGW <10 . We discuss the implication of gamma-ray limits that some high energy sources may be highly polarized (thus on the characteristics of the gravitational wave source, based on the improving our chances of a making useful measurements), and the available predictions for prompt electromagnetic emission. ready availability of modern computing resources that provide the 1 7 ability to carry out more comprehensive simulations in support of Author(s): Volodymyr Savchenko , Carlo Ferrigno , Sandro Mereghetti5667 , Lorenzo Natalucci , Angela Bazzano , Enrico Bozzo , the analysis. The only significant work done to date with regards to 72 8 COMPTEL polarimetry was published almost 20 years ago and Thierry J.-L. Courvoisier , Soren Brandt , Lorraine Hanlon , Erik Kuulkers311 , Philippe Laurent , François Lebrun , Jean-Pierre used a simplified mass model of COMPTEL for simulating the 96 4 instrument response. Estimates of the minimum detectable Roques , Pietro Ubertini , Georg Weidenspointner polarization (MDP) near 1 MeV included 30% for a two-week Institution(s): 1. APC, Universite Paris Diderot, CNRS/IN2P3, observation of the Crab, as low as 10% for bright GRBs, and as low CEA/Irfu, Observatoire de Paris, 2. DTU Space - National Space as 10% for bright solar flares. The data analysis performed at the Institute Elektrovej, 3. European Space Astronomy Centre time led to inconclusive results and suggested some unknown (ESA/ESAC), Science Operations Department 28691, 4. European systematic error. We contend that a self-consistent analysis will be XFEL GmbH, 5. IASF-Milano, 6. INAF-Institute for Space feasible with high fidelity simulations, simulations that were not Astrophysics and Planetology, 7. ISDC, Department of astronomy, easily generated 20 years ago. Our analysis utilizes the latest University of Geneva, 8. Space Science Group, School of Physics, GEANT4 simulation tools in conjunction with a high-fidelity mass University College Dublin, 9. Universite Toulouse; UPS-OMP; model of the COMPTEL instrument, and incorporate updated CNRS; IRAP 113.04 – Exploring Gravitational Waves in the Author(s): Robert Frederic Archibald6, Victoria M. Kaspi6 , Classroom Andrew P Beardmore11 , Neil Gehrels 3 , Jamie Kennea 7 , Eric V. Gotthelf26 , Robert Ferdman , Sebastien Guillot 81 , Fiona Harrison , On September 14, 2015, the Laser Interferometer Evan Keane954 , Michael Pivovaroff , Daniel Stern , Shriharsh P. Gravitational-wave Observatory (LIGO) received the first Tendulkar610 , John Tomsick confirmed gravitational wave signals. Now known as GW150914 Institution(s): 1. Cahill Center for Astrophysics, 2. Columbia (for the date on which the signals were received), the event Astrophysics Laboratory, 3. Goddard Space Flight Center, 4. Jet represents the coalescence of two black holes that were previously Propulsion Laboratory, 5. Lawrence Livermore National in mutual orbit. LIGO’s exciting discovery provides direct evidence Laboratory, 6. McGill, 7. Pennsylvania State University, 8. of what is arguably the last major unconfirmed prediction of Pontificia Universidad Catolica de Chile, 9. SKA Organisation, 10. Einstein’s General Theory of Relativity. The Education and Public Space Science Laboratory, 11. University of Leicester Outreach group at Sonoma State University has created an educator's guide that provides a brief introduction to LIGO and to gravitational waves, along with two simple demonstration activities 114.04 – Polar Cap Pair Production for an that can be done in the classroom to engage students in Axisymmetric Pulsar Requires General Relativity understanding LIGO’s discovery. Additional resources have also Using an analytical approach coupled to a condition for pair been provided to extend student explorations of Einstein’s production derived from particle in cell simulations, we show that Universe. pair production by curvature photons on magnetic field lines at the polar cap is inactive if general relativity is ignored. In particular, Author(s): Lynn R. Cominsky1, Kevin M. McLin1 , Carolyn general relativisitic frame-dragging lowers the value of the Peruta11 , Aurore Simonnet Goldreich-Julian density at the polar cap compared to its value for a Institution(s): 1. Sonoma State Univ. flat spacetime. This leads to a region of space-like current near the surface of the neutron star where pair production is possible.

114 – Isolated Nss Poster Session However, even when general relativity is included, we show analytically that pair production on magnetic field lines is 114.01 – Evolution of the X-ray Properties of the suppressed near the outer edge of the polar cap. This leads to the Transient Magnetar XTE J1810-197 possibility of a ``vacuum" region of unscreened parallel electric We report on X-ray observations of the 5.54 s transient magnetar field on open field lines near the last open field line. Such a vacuum XTE J1810-197 using the XMM-Newton and Chandra region has indeed been observed in particle in cell simulations of observatories, analyzing new data from 2008 through 2014, and the pulsar magnetosphere. re-analyzing data from 2003 through 2007 with the benefit of these six years of new data. From the discovery of XTE J1810-197 Because of the generality of our analytical approach (which does during its 2003 outburst to the most recent 2014 observations, its not assume a dipolar surface field), our conclusions are true 0.3-10 keV X-ray flux has declined by a factor of about 50 from independent of the detailed structure of the magnetic field at the 4.1E-11 to 8.1E-13 erg/cm^2/s. Its X-ray spectrum has now surface of the neutron star. We confirm our analytical results by reached a steady state. Pulsations continue to be detected from a comparing them to force-free simulations of a pulsar with a dipolar 0.3 keV thermal hot-spot that remains on the neutron star surface. surface field. The luminosity of this hot-spot exceeds XTE J1810-197's spin 1 down luminosity, indicating continuing magnetar activity. We find Author(s): Mikhail Belyaev that XTE J1810-197's X-ray spectrum is best described by a Institution(s): 1. UC Berkeley multiple component blackbody model in which the coldest 0.14 keV component likely originates from the entire neutron star 114.05 – Young gamma-ray pulsar: from modeling the surface, and the thermal hot-spot is, at different epochs, well gamma-ray emission to the particle-in-cell described by an either one or two-component blackbody model. A simulations of the global magnetosphere 1.2 keV absorption line, possibly due to resonant proton scattering, is detected at all epochs. The X-ray flux of the hot spot decreased by Accelerated charged particles flowing in the magnetosphere approximately 20% between 2008 March and 2009 March, the produce pulsar gamma-ray emission. Pair creation processes same period during which XTE J1810-197 became radio quiet. produce an electron-positron plasma that populates the magnetosphere, in which the plasma is very close to force-free. Author(s): Jason Alford1 However, it is unknown how and where the plasma departs from Institution(s): 1. Columbia University the ideal force-free condition, which consequently inhibits the understanding of the emission generation. We found that a 114.02 – Unusual Braking Indices in Young X-ray dissipative magnetosphere outside the light cylinder effectively Pulsars reproduces many aspects of the young gamma-ray pulsar emission Pulsars spin down over time. By measuring braking indices of as seen by the Fermi Gamma-ray Space Telescope, and through pulsars, effectively the change in the spin-down rate over time, we particle-in-cell simulations (PIC), we started explaining this can probe the underlying driving engine of the spin-down. For a configuration self-consistently. These findings show that, together, magnetic dipole in a vacuum, n is predicted to be 3. To date, all a magnetic field structure close to force-free and the assumption of measured braking indices are less than 3, which can be explained, gamma-ray curvature radiation as the emission mechanism are e.g. by particle winds, changes in the magnetic field. In all models strongly compatible with the observations. Two main issues from of braking indices, n should be nearly constant on year time-scales. the previously used models that our work addresses are the Here, I will discuss two recent observation results that challenge inability to explain luminosity, spectra, and light curve features at this model, interestingly both coming from young X-ray pulsars the same time and the inconsistency of the electrodynamics. with no detected radio emission. The first, a long-lived decrease in Moreover, using the PIC simulations, we explore the effects of the braking index of PSR J1846-0258 following a burst of different pair multiplicities on the magnetosphere configurations magnetar-like activity, and secondly, the first stationary braking and the locations of the accelerating regions. Our work aims for a index greater than three. Understanding neutron-star spin self-consistent modeling of the magnetosphere, connecting the evolution is key to constraining these objects' long-term energy microphysics of the pair-plasma to the global magnetosphere output and has relevance to topics ranging from pulsar wind macroscopic quantities. This direction will lead to a greater nebulae and supernova remnants to core-collapse supernova rates, understanding of pulsar emission at all wavelengths, as well as to physics, and expected outcomes. concrete insights into the physics of the magnetosphere. Author(s): Gabriele Brambilla2, Constantions MSPs detected by a group of thirteen radio surveys as well as the Kalapotharakos11 , Andrey Timokhin , Alice Kust Harding 1 , MSP birth rate in the Galaxy and the number of MSPs detected by Demosthenes Kazanas1 Fermi. We explore various high-energy emission geometries like Institution(s): 1. NASA Goddard Space Flight Center, 2. the slot gap, outer gap, two pole caustic and pair starved polar cap University of Milan models. The parameters associated with the birth distributions for the mass accretion rate, magnetic field, and period distributions are 114.06 – NICER observation of magnetars well constrained. With the set of four free parameters, we employ The Neutron Star Interior Composition ExploreR (NICER) is a Markov Chain Monte Carlo simulations to explore the model NASA Explorer Misson of Opportunity as an attached payload parameter space. We present preliminary comparisons of the aboard the International Space Station (ISS), launch in August simulated and detected distributions of radio and gamma-ray 2016. The NICER is planned to study the interior composition and pulsar characteristics. We estimate the contribution of MSPs to the structure within neutron stars via high precise measurement of diffuse gamma-ray background with a special focus on the Galactic their stellar mass and radius, also to investigate dynamic and Center. energetic behaviors of their activities. This mission will enable We express our gratitude for the generous support of the National pulsar rotation-resolved spectroscopy in the 0.2--12 keV energy Science Foundation (RUI: AST-1009731), Fermi Guest Investigator band with large collection area (about twice of the XMM-Newton Program and the NASA Astrophysics Theory and Fundamental observatory for soft X-ray timing), precise time-tagging resolution Program (NNX09AQ71G). (~200 nsec, 25 times better than RXTE), and high sensitivity Author(s): Peter L. Gonthier1, Yew-Meng Koh1 , Alice Kust (about 2e-14 erg/s/cm2 in the 0.5--10 keV, 5-sigma for 10 ksec 2 exposure). As one of prime goals of the mission, we will describe Harding the science planning of the NICER magnetar observations. The Institution(s): 1. Hope College, 2. NASA Goddard Space Flight NICER is expected to provide monitoring of fainter magnetar Center sources which cannot be performed by Swift due to its little collective area. Deep observations of quiescent magnetars and 114.09 – Lastest Results from the X-ray Monitoring high-B radio pulsars can be also performed with the NICER to Campaign of AXP CXOU J17145.7-381031 in CTB 37B study their spectral similarity as a key to investigate the connection The 3.82 s AXP CXOU J17145.7-381031 in the supernova remnant between these two sub-classes. Finally, ToO programs are suitable CTB 37B has one of the largest spin-down powers for a magnetar, to follow-up the magnate outburst relaxation down to much fainter and it may be the youngest one as well. Magnetars with the greatest flux level. We will introduce the NICER strategy of the magnetar spin-down power are SGRs, and a marked increase in their observation. spin-down torque often preceds an outburst. In this regard, AXP CXOU J17145.7-381031 is very similar to SGR/AXP 1E Author(s): Teruaki Enoto1, Victoria M. Kaspi2 , Zaven 1547.0-5408, the magnetar with the largest spin-down power. We Arzoumanian3 will report on the latest timing and spectral results from our Institution(s): 1. Kyoto University, 2. McGill University, 3. on-going Chandra and XMM X-ray monitoring campaign on the NASA/GSFC AXP in CTB 37B. We also present a NuSTAR observation that reveals a separate, hard spectral component similar to that found 114.07 – A Magnetar Wind Nebula: the Spin-down- for other magnetars. Powered Wind is not Enough 1 1 Magnetars are a small class of slowly-rotating (P~2-12 s) highly Author(s): Eric V. Gotthelf , Jules P. Halpern magnetized (surface dipole fields ~10^{14}-10^{15} G) that show a Institution(s): 1. Columbia Astrophysics Lab. variety of bursting activity, powered by the decay of their super- strong magnetic field. While many rotation-powered pulsars are 114.10 – Chandra Phase-Resolved Spectroscopy of the surrounded by a pulsar wind nebula (PWN) powered by their High-Magnetic-Field Pulsar B1509-58 spin-down MHD wind (the prime example being the Crab nebula), We report on timing and spectral analysis of the young, only now has the first magnetar wind nebula (MWN) been high-magnetic-field pulsar B1509-58 using Chandra continuous- discovered in X-rays, around Swift J1834.9-0846. We have clocking mode observation. The on-pulsed X-ray spectrum can be analyzed this system in detail to see what can be learned from it. described by a power law with a photon index of 1.16(2), which is We find good evidence that unlike normal PWNe, this MWN flatter than those determined with RXTE/PCA and NuSTAR. This cannot be powered by its spin-down MHD wind alone. A result supports the log-parabolic model for the broadband X-ray considerable contribution to the MWN energy should come from a spectrum. With the unprecedented angular resolution of Chandra, different source, most likely sporadic outflows associated with the we clearly identified off-pulsed X-ray emission from the pulsar. magnetar's bursting activity. This suggests that the MWN may The spectrum is best fitted by a power law plus blackbody model. serve as a calorimeter, and provide a new and robust estimate for The latter component has a temperature of ~0.14 keV, which is the magnetar's long-term mean energy output rate in outflows. We similar to those of other young and high-magnetic-field pulsars, also discuss other interesting aspects of this system. and lies between those of magnetars and typical rotational-powered pulsars. For the non-thermal emission of PSR B1509-58, we found Author(s): Ramandeep Gill6, Jonathan Granot6 , Matthew G. that the power law component of the off-pulsed emission is Baring43 , Joseph Gelfand , George A. Younes 55 , Oleg Kargaltsev , significantly steeper than that of the on-pulsed one. We further Alice Kust Harding15 , Chryssa Kouveliotou , Daniela divided the data into 24 phase bins and found that the photon Huppenkothen2 index varies between 1.0 and 2.0 and anti-correlating with the flux. Institution(s): 1. NASA/GSFC, 2. New York University, 3. New A similar correlation was also found in the Crab Pulsar, and this York University Abu Dhabi, 4. Rice University, 5. The George requires further theoretical interpretations. This work is supported Washington University, 6. The Open University of Israel by a GRF grant of Hong Kong Government under 17300215.

114.08 – Population synthesis of radio and gamma-ray Author(s): Chin-Ping Hu1, Chi-Yung Ng1 millisecond pulsars using Markov Chain Monte Carlo Institution(s): 1. The University of Hong Kong techniques We present preliminary results of a new population synthesis of 114.11 – Fermi γ-ray Pulsars: Towards the millisecond pulsars (MSP) from the Galactic disk using Markov Understanding of the Pulsed High-Energy Emission Chain Monte Carlo techniques to better understand the model Based on the Fermi observational data we reveal meaningful parameter space. We include empirical radio and gamma-ray constraints for the dependence of the macroscopic parameters of luminosity models that are dependent on the pulsar period and dissipative pulsar magnetosphere models on the corresponding period derivative with freely varying exponents. The magnitudes of spin-down rate. Our models are specifications of the FIDO the model luminosities are adjusted to reproduce the number of (Force-Free Inside, Dissipative Outside) model where the dissipative regions are outside the light-cylinder near the equatorial strong orbital variation, about 5 times greater than is typical for current sheet. These models provide not only the field geometry other systems, and is also very clearly double peaked. Hints of but also the necessary particle accelerating electric fields. Assuming similar peaks have been observed in the lightcurves of other emission due to curvature radiation, the FIDO models reproduce redback systems, and so this system can help in understanding the the observed light-curve phenomenology as depicted in the intrabinary shock of eclipsing MSPs. radio-lag vs peak-separation diagram obtained by Fermi. A direct and detailed comparison of the model spectral properties (cutoff Author(s): Hind Al Noori2, Mallory Roberts21 , Jason Hessels , energies and total γ-ray luminosities) with those observed by Fermi Maura McLaughlin43 , Rene Breton reveals the dependence of the macroscopic conductivity parameter Institution(s): 1. Astron, 2. New York University Abu Dhabi, 3. on the spin-down rate providing a unique insight for the University of Manchester, 4. West Virginia University understanding of the physical mechanisms behind the high-energy emission in pulsar magnetospheres. 115 – Laboratory Astrophysics and Data Author(s): Constantinos Kalapotharakos1, Alice Kust Harding111 , Demosthenes Kazanas , Gabriele Brambilla Analysis Poster Session Institution(s): 1. NASA, Goddard Space Flight Center 115.01 – Charge Exchange, from the Laboratory to 114.14 – The 3D Space and Spin Velocities of a Galaxy Clusters Gamma-ray Pulsar X-ray emission due to charge exchange (CX) between solar wind ions and neutrals in comets and planetary atmospheres is PSR J2030+4415 is a LAT-discovered 0.5My-old gamma-ray ubiquitous in the solar system, and is also a significant foreground pulsar with an X-ray synchrotron trail and a rare Halpha bowshock. in all observations from low-Earth orbit. It is also possible that CX We have obtained GMOS IFU spectroscopic imaging of this shell, is common astrophysically, in any environment where hot plasma and show a sweep through the remarkable Halpha structure, and cold gas interact. A current challenge is that theoretical models comparing with the high energy emission. These data provide a of CX spectra do not always accurately describe observations, and unique 3D map of the momentum distribution of the relativistic require further experimental verification. This is especially pulsar wind. This shows that the pulsar is moving nearly in the important to focus on now, as the recent launch of Astro-H is plane of the sky and that the pulsar wind has a polar component providing us with the first high-resolution spectra of extended misaligned with the space velocity. The spin axis is shown to be x-ray sources. In order to improve our understanding and inclined some 95degrees to the Earth line of sight, explaining why modeling of CX spectra, we take advantage of the laboratory this is a radio-quiet, gamma-only pulsar. Intriguingly, the shell also astrophysics program at the Lawrence Livermore National shows multiple bubbles that suggest that the pulsar wind power Laboratory and use an Electron Beam Ion Trap (EBIT) to perform has varied substantially over the past 500 years. CX experiments, using the EBIT Calorimeter Spectrometer. We Author(s): Roger W. Romani1 present experimental benchmarks that can be used to develop a Institution(s): 1. Stanford Univ. more comprehensive and accurate CX theory. On the observational side, we also investigate the possibility of CX occurring in the filaments around the central galaxy of the Perseus cluster, NGC 114.16 – Pulsars at the Center of the Galaxy 1275. We use Chandra ACIS data, combined with what we know Over the past few years, a number of groups using data from about laboratory CX spectra, to investigate the possibility of CX NASA’s space-borne Fermi LAT instrument have identified excess being a significant contributor to the x-ray emission. gamma-ray flux toward the inner few degrees of the Galactic Center (GC), with an even larger significant excess within 1 degree of this Author(s): Gabriele Betancourt-Martinez31 , Peter Beiersdorfer , region. At present there are two leading candidates for this excess: Gregory Brown11 , Natalie Hell , Maurice A. Leutenegger 2 , dark matter annihilation and a population of unresolved Frederick S Porter23 , Christopher S. Reynolds millisecond pulsars (MSPs). We are currently developing dedicated Institution(s): 1. Lawrence Livermore National Laboratory, 2. instrumentation to carry out a sensitive search for the pulsars in NASA/Goddard Space Flight Center, 3. University of Maryland, this region of the galaxy using a newly developed front end and College Park receiver on a Deep Space Network large diameter antenna in Australia. In this presentation, we will provide an overview of the 115.02 – XSPEC and PyXSPEC challenges encountered with pulsar searches at the GC region and a I will describe recent changes and planned improvements for summary of previous and ongoing efforts to survey this region with XSPEC and PyXspec. radio telescopes. We will also provide preliminary results from our recent observations of the GC region at 2 and 8 GHz and will Author(s): Keith A. Arnaud1 conclude with prospects for detection of perhaps hundreds of Institution(s): 1. CRESST/UMd/GSFC pulsars in this region with new generations of radio telescopes now under construction.

Author(s): Walid A. Majid1 116 – Missions & Instruments Poster Session Institution(s): 1. JPL/Caltech 116.01 – The Transient High Energy Sky and Early Universe Surveyor 114.17 – X-ray studies of the redback system PSR J2129-0429 The Transient High Energy Sky and Early Universe Surveyor is a mission which will be proposed for the ESA M5 call. THESEUS will We present new NuStar data of the redback millisecond pulsar address multiple components in the Early Universe ESA Cosmic (MSP) system PSR J2129-0429. Redback systems are important Vision theme: when it comes to understanding the evolution of MSPs, in terms of 4.1 Early Universe, pulsar recycling, as they have been observed to transition between 4.2 The Universe taking shape, and a state of accretion, where emission is in the optical and X-ray 4.3 The evolving violent Universe. regimes, and a state of eclipsed radio pulsation. This system is particularly interesting due to some peculiarities: it has a more THESEUS aims at vastly increasing the discovery space of the high massive companion as well as a stronger magnetic field than other energy transient phenomena over the entire cosmic history. This is redbacks, indicating that the system is in a fairly early stage of achieved via a unique payload providing an unprecedented recycling. It’s X-ray lightcurve (as obtained from XMM-Newton combination of: (i) wide and deep sky monitoring in a broad energy data) has a very hard power-law component and exhibits an band(0.3 keV-20 MeV; (ii) focusing capabilities in the soft X-ray efficiency of a few percent in X-ray. With the NuStar data, the band granting large grasp and high angular resolution; and (iii) on spectrum can be seen to extend to ~30 keV. Additionally, it shows board near-IR capabilities for immediate transient identification and first redshift estimate. 122 keV gamma rays in the laboratory. In addition of experimental works, we have been working on gamma ray tracing model of the The THESEUS payload consists of: (i) the Soft X--ray Imager concentrator by IDL, making use of optical properties calculated by (SXI), a set of Lobster Eye (0.3--6 keV) telescopes with CCD the IMD software. This modeling allows us to calculate efficiency detectors covering a total FOV of 1 sr; (ii) the X--Gamma-rays and focal length for different energy bands and materials and spectrometer (XGS), a non-imaging spectrometer (XGS) based on compare them with experimental result. Also we will combine SDD+CsI, covering the same FOV than the Lobster telescope concentrator modeling result and detector simulation by Geant4 to extending the THESEUS energy band up to 20 MeV; and (iii) a archive a complete package of gamma-ray telescope simulation. If 70cm class InfraRed Telescope (IRT) observing up to 2 microns successful, this technology will offer the potential for soft with imaging and moderate spectral capabilities. gamma-ray telescopes with focal lengths of less than 10 m, removing the need for formation flying spacecraft and opening the The main scientific goals of THESEUS are to: field up to balloon-borne instruments and providing greatly (a) Explore the Early Universe (cosmic dawn and reionization era) increased sensitivity for modest cost and complexity. by unveiling the Gamma--Ray Burst (GRBs) population in the first billion years}, determining when did the first stars form, and Author(s): Farzane Shirazi5, Peter F. Bloser5 , Paul H. investigating the re-ionization epoch, the interstellar medium Aliotta22 , Olof Echt , James E. Krzanowski 4 , Jason S Legere 5 , (ISM) and the intergalactic medium (IGM) at high redshifts. Mark L. McConnell541 , John G. Tsavalas , Emily N. Wong , R. Marc Kippen3 (b) Perform an unprecedented deep survey of the soft X-ray Institution(s): 1. Department of Chemical Engineering, transient Universe in order to fill the present gap in the discovery University of New Hampshire, 2. Department of Physics, space of new classes of transient; provide a fundamental step University of New Hampshire, 3. Los Alamos National forward in the comprehension of the physics of various classes of Laboratory, 4. Materials Science Program, University of New Galactic and extra--Galactic transients, and provide real time trigger Hampshire, 5. Space Science Center, University of New Hampshire and accurate locations of transients for follow-up with next-generation facilities. 116.04 – Analysis of Data from the Balloon Borne Gamma RAy Polarimeter Experiment (GRAPE) (c) Provide IR survey capabilities in space and strong guest The Gamma Ray Polarimeter Experiment (GRAPE), a balloon observer possibilities, thus allowing a strong community borne polarimeter for 50~300 keV gamma rays, successfully flew involvement. All transient alerts will be public. in 2011 and 2014. The main goal of these balloon flights was to measure the gamma ray polarization of the Crab Nebula. Analysis 1 Author(s): P. T. O'Brien of data from the first two balloon flights of GRAPE has been Institution(s): 1. University of Leicester challenging due to significant changes in the background level during each flight. We have developed a technique based on the 116.02 – Laboratory demonstration of the Principle Component Analysis (PCA) to estimate the background piezoelectric figure correction of a cylindrical for the Crab observation. We found that the background depended slumped glass optic mostly on the atmospheric depth, pointing zenith angle and The X-ray Surveyor is a mission concept for a next generation instrument temperatures. Incorporating Anti-coincidence shield X-ray observatory. This mission will feature roughly 30 times the data (which served as a surrogate for the background) was also effective area of the Chandra Observatory while matching its found to improve the analysis. Here, we present the calibration sub-arcsecond angular resolution. The key to meeting these data and describe the analysis done on the GRAPE 2014 flight data. requirements is lightweight, segmented optics. To ensure these optics achieve and maintain sub-arcsecond performance, we Author(s): Sambid K Wasti1, Peter F. Bloser1 , Jason S propose to use piezoelectric coatings for post-bonding and on-orbit Legere111 , Mark L. McConnell , James M. Ryan figure correction. We have fabricated a cylindrical prototype optic Institution(s): 1. University of New Hampshire with piezoelectric adjusters and measured its performance using optical metrology. We present the results of this laboratory figure 116.05 – Polarization from Relativistic Astrophysical correction and discuss their implications for an observatory X-ray Sourses: The PRAXyS Small Explorer featuring adjustable X-ray optics. Observatory Polarization is a sensitive probe of geometry near compact objects, 3 33 Author(s): Ryan Allured , Edward Hertz , Vanessa Marquez , but remains largely unexplored in the X-ray band. Polarization is Vincenzo Cotroneo321 , Margeaux L Wallace , Bianca Salmaso , 123expected from cosmic X-ray sources, yielding insight into the Marta M Civitani , Susan Trolier-McKinstry , Alexey Vikhlinin , geometry of black hole emission, and the origin and nature of 13 Giovanni Pareschi , Paul B. Reid X-ray emission in neutron stars and magnetars. Recent progress Institution(s): 1. Osservatorio Astronomico di Brera, 2. with detectors capable of imaging the track of a photoelectron Pennsylvania State University, 3. Smithsonian Astrophysical generated by a detection of a cosmic X-ray have made sensitive Observatory X-ray polarization observatories possible within the constraints of a NASA Small Explorer mission. We report on the observational 116.03 – Simulation and Optimization of Soft capabilities and the scientific goals of the "Polarization from Gamma-Ray Concentrator Using Thin Film Multilayer Relativistic Astrophysical X-ray Sources" (PRAXyS) Observatory. Structures PRAXyS is a small explorer which has been selected by NASA for a We are reporting the investigation result of channeling and phase A study. concentrating soft gamma rays (above 100 keV) using multilayer thin films of alternating low and high-density materials. This will Author(s): Timothy R. Kallman2, Keith Jahoda2 , Chryssa enable future telescopes for higher energies with same mission Kouveliotou12 , The PRAXyS Team parameters already proven by NuSTAR. Base on initial Institution(s): 1. George Washington University, 2. NASA/GSFC investigations at Los Alamos National Laboratory (LANL) we are investigating of producing these multilayers with the required 116.06 – Second launch of the Diffuse X-ray emission thicknesses and smoothness using magnetron sputter (MS) and from the Local Galaxy (DXL) mission pulsed laser deposition (PLD) techniques. A suitable arrangement The Diffuse X-ray emission from the Local Galaxy (DXL) is a of bent multilayer structures of alternating low and high-density sounding rocket mission to study the Solar Wind Charge Exchange materials will channel soft gamma-ray photons via total external (SWCX) and Local Hot Bubble (LHB) X-ray emission. After a reflection and then concentrate the incident radiation to a point. successful launch of December 2012, DXL’s capabilities were The high-energy astrophysics group at the UNH Space Science expanded by using two additional proportional counters and three Center (SSC) is testing these structures for their ability to channel unique filters for the launch of December 2015. Employing Be-, B- and C-based plastic filters, DXL mission re-scanned the Helium spectrometer with high resolving power and extended Focusing Cone for better spectral and positional information (to bandpass address the IBEX controversy). In this paper, we will review the A number of high priority questions in astrophysics can be upgraded mission hardware and performance, while sharing some addressed by a state-of-the-art soft x-ray grating spectrometer, preliminary results from the latest observation. such as the role of Active Galactic Nuclei in galaxy and star formation, characterization of the Warm-Hot Intergalactic Medium Submitted for the DXL Collaboration and the “missing baryon” problem, characterization of halos around the Milky Way and nearby galaxies, as well as stellar Author(s): Dhaka Mohan Sapkota1 coronae and surrounding winds and disks. An Explorer-scale, Institution(s): 1. University of Miami large-area (> 1,000 cm2 ), high resolving power (R = λ/Δλ > 3,000) soft x-ray grating spectrometer is highly feasible based on 116.08 – Compton-Pair Production Space Telescope Critical-Angle Transmission (CAT) grating technology. Still (ComPair) for MeV Gamma-ray Astronomy significantly higher performance can be provided by a CAT grating The gamma-ray energy range from a few hundred keV to a few spectrometer on an X-ray-Surveyor-type mission. CAT gratings hundred MeV has remained largely unexplored, mainly due to the combine the advantages of blazed reflection gratings (high challenging nature of the measurements, since the pioneering, but efficiency, use of higher diffraction orders) with those of limited, observations by COMPTEL on the Compton Gamma-Ray conventional transmission gratings (low mass, relaxed alignment Observatory (1991- 2000). This energy range is a transition region tolerances and temperature requirements, transparent at higher between thermal and nonthermal processes, and accurate energies) with minimal mission resource requirements. They are measurements are critical for answering a broad range of high-efficiency blazed transmission gratings that consist of astrophysical questions. We are developing a MIDEX-scale freestanding, ultra-high aspect-ratio grating bars fabricated from wide-aperture discovery mission, ComPair (Compton-Pair silicon-on-insulator (SOI) wafers using advanced anisotropic dry Production Space Telescope), to investigate the energy range from and wet etch techniques. Blazing is achieved through grazing- 200 keV to > 500 MeV with high energy and angular resolution incidence reflection off the smooth grating bar sidewalls. The and with sensitivity approaching a factor of 100 better than reflection properties of silicon are well matched to the soft x-ray COMPTEL. This instrument will be equally capable to detect both band. Nevertheless, CAT gratings with sidewalls made of higher Compton-scattering events at lower energy and pair-production atomic number elements allow extension of the CAT grating events at higher energy. ComPair will build on the heritage of principle to higher energies and larger dispersion angles. We show successful space missions including Fermi LAT, AGILE, AMS and x-ray data from metal-coated CAT gratings and demonstrate PAMELA, and will utilize well-developed space-qualified detector efficient blazing to higher energies and larger blaze angles than technologies including Si-strip and CdZnTe-strip detectors, heavy possible with silicon alone. We also report on measurements of the inorganic scintillators, and plastic scintillators. resolving power of a breadboard CAT grating spectrometer consisting of a Wolter-I slumped-glass focusing mirror pair from Author(s): Alexander Moiseev1 Goddard Space Flight Center and CAT gratings, to be performed at Institution(s): 1. NASA/GSFC and University of Maryland the Marshall Space Flight Center Stray Light Facility.

116.09 – Proposal of balloon and satellite observations Author(s): Ralf K. Heilmann2, Alexander Robert Bruccoleri1 , of MeV gammas using Electron Tracking Compton Mark Schattenburg2 Camera for reaching a high sensitivity of 1 mCrab Institution(s): 1. Izentis LLC, 2. MIT ETCC with a gas Time Projection Chamber (TPC) and pixel GSO scintillators, by measuring electron tracks precisely, provides both 116.11 – Cross-calibration of the CCD Instruments a strong background rejection by dE/dx of the track and onboard the Chandra, Suzaku, Swift, and well-defined 2-dimensional Point Spread Function (PDF) with XMM-Newton Observatories using 1E 0102.2-7219 better than several degrees by adding the arc direction of incident We report on our continuing efforts to compare the gammas (SPD: Scatter Plane Deviation) with the ARM (angular time-dependent calibrations of the current generation of CCD Resolution Measure) direction measured in standard Compton instruments onboard the Chandra, Suzaku, Swift, and Camera (CC). In 2006 its background rejection was revealed by XMM-Newton observatories using the brightest supernova SMILE-I balloon experiment with 10cm-cubic ETCC using the remnant in the Small Magellanic Cloud, 1E 0102.2-7219 (hereafter dE/dx of tracks. In 2013, 30cm-cube-ETCC has been developed to E0102). This calibration is a function of time due to the effects of catch gammas from Crab in next SMILE-II balloon with >5sigma radiation damage on the CCDs and the accumulation of a detection for 4 hrs. Now its sensitivity has been improved to contamination layer on the filters or CCDs. We desire a simple 10sigma by attaining the angular resolution of the track (SPD comparison of the absolute effective areas in the 0.5-1.0 keV angle) to that determined by multiple scattering of the gas. Thus, bandpass. The spectrum of E0102 has been well-characterized we show the ability of ETCC to give a better significance by a factor using the RGS grating instrument on XMM-Newton and the HETG of 10 than that of standard CCs having same detection area by grating instrument on Chandra. We have developed an empirical electron tracking?and we have found that SPD is an essential to model for E0102 that includes Gaussians for the identified lines, define the PSF of Compton imaging quantitatively. Such a two absorption components, and two continuum components with well-defined PSF is, for the first time, able to provide reliable different temperatures. In our fits, the model is highly constrained sensitivity in Compton imaging without assuming the use of in that only the normalizations of the four brightest line complexes optimization algorithm. These studies uncover the uncertainties of (the O VII triplet, the O VIII Ly-alpha line, the Ne IX triplet, and CCs from both points of view of the intense background and the the Ne X Ly-alpha line) and an overall normalization are allowed to difficulty of the definition of the PSF, and overcome the above vary. In our previous study, we found that based on observations problems. Based on this technology, SMILE-II with 3atm CF4 gas early in the missions, most of the fitted line normalizations agreed is expected to provide a 5times better sensitivity than COMPTEL in to within +/- 10%. We have now expanded this study to include one month balloon, and 4modules of 50cm-cube ETCCs would more recent data from these missions using the latest calibration exceed over 10^-12 erg/cm^2s^1 (1mCrab) in satellite. Here we updates and we will report on the current level of agreement summarize the performance of the ETCC and new astrophysics amongst these instruments. opened in near future by high sensitive observation of MeV gamma-rays. This work is based on the activities of the International Astronomical Consortium for High Energy Calibration (IACHEC). Author(s): Atsushi Takada1, Toru Tanimori1 Institution(s): 1. Kyoto University

116.10 – Soft x-ray blazed transmission grating Author(s): Paul P. Plucinsky2 , Andrew P Beardmore6 , Adam Author(s): Paul B. Reid111 , Ryan Allured , Sagi ben-Ami , Foster2354 , Matteo Guainazzi , Frank Haberl , Eric Miller , Andrew Vincenzo Cotroneo11 , Daniel A. Schwartz , Harvey Tananbaum 1 , Pollock16 , Steve Sembay , Martin Stuhlinger 1 Alexey Vikhlinin12 , Susan Trolier-McKinstry , Margeaux L Institution(s): 1. ESAC, 2. Harvard-Smithsonian, CfA, 3. JAXA, Wallace22 , Tom Jackson 4. MIT, 5. MPE, 6. University of Leicester Institution(s): 1. Harvard-Smithsonian Center for Astrophysics, 2. The Pennsylvania State University 116.12 – Lessons Learned Designing and Building the Chandra Telescope 116.16 – The HEASARC in 2016: 25 Years and Counting This poster offers some of the major lessons learned by key The High Energy Astrophysics Archival Research Center or members of the Chandra Telescope team. These lessons are HEASARC (http://heasarc.gsfc.nasa.gov/) has been the NASA gleaned from our experiences developing, designing, building and astrophysics discipline archive supporting multi-mission cosmic testing the telescope and its subsystems, with 15 years of hindsight. X-ray and gamma-ray astronomy research for 25 years, and, Among the topics to be discussed are the early developmental tests, through its LAMBDA (Legacy Archive for Microwave Background known as VETA-I and VETA-II, requirements derivation, the Data Analysis: http://lambda.gsfc.nasa.gov/) component, the impact of late requirements and reflection on the conservatism in archive for cosmic microwave background data for the last 8 years. the design process. This poster offers some opinions on how these The HEASARC is the designated archive which supports NASA's lessons can affect future missions. Physics of the Cosmos theme (http://pcos.gsfc.nasa.gov/).

Author(s): Jonathan Arenberg1 The HEASARC provides a unified archive and software structure Institution(s): 1. Northrop Grumman aimed both at 'legacy' high-energy missions such as Einstein, EXOSAT, ROSAT, RXTE, and Suzaku, contemporary missions 116.13 – Low energy response of the NICER detectors such as Fermi, Swift, XMM-Newton, Chandra, NuSTAR, etc., and and "threshold efficiency" effect upcoming missions, such as Astro-H and NICER. The HEASARC's The Neutron Star Interior Composition ExploreR (NICER) is an high-energy astronomy archive has grown so that it presently instrument that is planned to be installed on the International contains more than 80 terabytes (TB) of data from 30 past and Space Station in 2016 to study time-resolved spectra of the rapidly present orbital missions. The user community downloaded 160 TB changing celestial ojects. The focal plane of the instrument consists of high-energy data from the HEASARC last year, i.e., an amount of 56 Silicon Drift Detectors (SDDs). Signal from each SDD is fed to equivalent to twice the size of the archive. shaping amplifiers and triggering circuits that determine both amplitude and time of arrival for each "event". We discuss some of the upcoming new initiatives and Zero crossing timing circuit is used in order to suppress energy developments for the HEASARC, including the arrival of public dependent "time walk". That is done with a chain producing a data from the JAXA/NASA Astro-H mission, expected to have been derivative of the shaped signal, and the same chain detects launched in February 2016, and the NASA mission of opportunity threshold crossings marking the arrival of an X-ray photon. Higher Neutron Star Interior Composition Explorer (NICER), expected to noise of the differentiated signal leads to a somewhat extended be deployed in late summer 2016. We also highlight some of the band of signal amplitudes close to the threshold value, for which new software and web initiatives of the HEASARC, and discuss our detection efficiency is less than 100%. Detection efficiency in this plans for the next 3 years. area affects the low energy portion of the detector response, and is 1 1 very well described by an error function. We will present accurate Author(s): Stephen Alan Drake , Alan P. Smale measurements of this effect, show the consequences for the Institution(s): 1. NASA/GSFC instrument quantum efficiency and the shape of the response function and will describe the calibration procedures that would 116.17 – The Fermi Guest Investigator program: allow selection of optimal threshold values for each observation. Impactful Science and Groundbreaking Results As an all-sky surveyor, the science impact from the Fermi Author(s): Gregory Prigozhin1, John Doty21 , Beverly LaMarr , Gamma-ray Space Telescope is limited by the number of scientists Andrew Malonis113 , Ronald A. Remillard , Frank Scholze , Christian performing data analysis, and not by the number of objects Laubis33 , Michael Krumrey observed by the spacecraft. To encourage this, the Fermi guest Institution(s): 1. MIT, 2. Noqsi Aerospace, 3. PTB investigator (GI) program supports a variety of scientific inquiries that benefit overall Fermi science. The GI program also provides 116.14 – Development Status of Adjustable X-ray access to radio, optical, X-ray and VHE gamma-ray data and/or Optics with 0.5 Arcsec Imaging for the X-ray Surveyor observing time, encouraging and enabling relevant multi- Mission Concept wavelength studies. This approach has allowed for new analyses The X-ray Surveyor mission concept is designed as a successor to and ideas to flourish, leading to world-class groundbreaking the Chandra X-ray Observatory. As currently envisioned, it will science and a number of unexpected discoveries. The program has have as much as 30-50 times the collecting area of Chandra with also supported a number of multi-year, multi-wavelength the same 0.5 arcsec imaging resolution. This combination of observing programs resulting in a rich variety of publicly available telescope area and imaging resolution, along with a detector suite resources. Here we describe the most significant results from the for imaging and dispersive and non-dispersive imaging Fermi GI program, including those resulting from both sky-survey spectroscopy, will enable a wide range of astrophysical and target of opportunity pointed observations. We discuss the observations. These observations will include studies of the growth public resources the program has supported, both for broad-band of large scale structure, early black holes and the growth of SMBHs, data acquisition and for the development of new analysis methods and high resolution spectroscopy with arcsec resolution, among and techniques. Additionally, we consider the ramifications of the many others. We describe the development of adjustable grazing existence of long-term multi-wavelength datasets, such as those incidence X-ray optics, a potential technology for the high enabled by the Fermi GI program, for future scientific inquiry. resolution, thin, lightweight mirrors. We discuss recent Author(s): Elizabeth C. Ferrara1 advancements including the demonstration of deterministic figure Institution(s): 1. NASA/GSFC correction via the use of the adjusters, the successful demonstration of integrating control electronics directly on the actuator cells to enable row-column addressing, and discuss the 116.18 – AtomDB and PyAtomDB: Atomic Data and feasibility of on-orbit piezoelectric performance and figure Modelling Tools for High Energy and Non-Maxwellian monitoring via integrated semiconductor strain gauges. We also Plasmas present the telescope point design and progress in determining the The release of AtomDB 3 included a large wealth of inner shell telescope thermal sensitivities and achieving alignment and ionization and excitation data allowing accurate modeling of mounting requirements. non-equilibrium plasmas. We describe the newly calculated data and compare it to published literature data. We apply the new this band, as well as being poised to discover new source types and models to existing supernova remnant data such as W49B and behaviors that have previously been unobservable. N132D. We further outline progress towards AtomDB 3.1, including a new energy-dependent charge exchange cross sections. Author(s): Elizabeth A. Hays1 Institution(s): 1. NASA/GSFC We present newly developed models for the spectra of electron- electron bremsstrahlung and those due to non-Maxwellian 116.22 – HaloSat: A CubeSat to Map the Distribution of electron distributions. Baryonic Matter in the Galactic Halo Approximately half of predicted baryonic matter in the Milky Way Finally, we present our new atomic database access tools, released remains unidentified. One possible explanation for the location of as PyAtomDB, allowing powerful use of the underlying this missing matter is in an extended Galactic halo. HaloSat is a fundamental atomic data as well as the spectral emissivities. CubeSat that aims to constrain the mass and distribution of the halo’s baryonic matter by obtaining an all-sky map of O VII and O Author(s): Adam Foster1, Randall K. Smith1 , Nancy S. 11 VIII emission in the hot gas associated with the halo of the Milky Brickhouse , Xiaohong Cui Way. HaloSat offers an improvement in the quality of Institution(s): 1. Harvard Smithsonian, CfA measurements of oxygen line emission over existing X-ray observatories and an observation plan dedicated to mapping the 116.19 – X-ray Reflection Gratings: Technology hot gas in the Galactic halo. In addition to the missing baryon Development Status Update problem, HaloSat will assign a portion of its observations to the We present the current status in the development of X-ray solar wind charge exchange (SWCX) in order to calibrate models of reflection gratings. Gratings mounted in the off-plane SCWX emission. We present here the current status of HaloSat configuration are capable of achieving high spectral resolving and the progression of instrument development in anticipation of a power concurrently with high diffraction efficiency. This will enable 2018 launch. key soft X-ray spectroscopy science goals to be achieved. We have identified hurdles to practically achieving the theoretical Author(s): Drew M Miles1 performance goals. Here we present our methodologies to Institution(s): 1. University of Iowa overcome these challenges. Furthermore, we discuss how we test these methods to quantify performance capabilities. The results of these tests are placed in the context of Technology Readiness Level 117 – Solar and Stellar Poster Session (TRL) in order to demonstrate our current status and to discuss our plans for the future. 117.01 – NuSTAR Search for Hard X-ray Emission from the Star Formation Regions in Sh2-104 1 Author(s): Randall L. McEntaffer We present NuSTAR hard X-ray observations of Sh2-104, a Institution(s): 1. University of Iowa compact Hii region containing several young massive stellar clusters (YMSCs). We have detected distinct hard X-ray sources 116.20 – Status of the Balloon-Borne X-ray coincident with localized VERITAS TeV emission recently resolved Polarimetry Mission X-Calibur from the giant gamma-ray complex MGRO J2019+37 in the We report on the status of the balloon borne hard X-ray Cygnus region. Faint, diffuse X-ray emission coincident with the polairmetry mission X-Calibur. The missions combines a focussing eastern YMSC in Sh2-104 is likely the result of colliding winds of hard X-ray mirror from the InFOCuS collaboration with a component stars. Just outside the radio shell of Sh2-104 lies scattering polarimeter and the WASP (Wallops Arc Second Pointer) 3XMM J201744.7+365045 and nearby nebula NuSTAR pointing system. The mission is scheduled for a conventonal ~1 day J201744.3+364812, whose properties are most consistent with balloon flight in Fall 2016 and a long duration (~30 day) balloon extragalactic objects. The combined XMM-Newton and NuSTAR flight from McMurdo (Ross Island) in 2018/2019. X-Calibur will spectrum of 3XMM J201744.7+365045 is well-fit to an absorbed allow us to measure ~5% polarization fractions for strong sources power-law model with NH = (3.1+/-1.0)E22 1/cm^2 and photon with a Crab-like enegry spectra and fluxes. The science targets of index Gamma = 2.1+/-0.1. Based on possible long-term flux the first balloon flights will include the stellar mass black holes variation and lack of detected pulsations (<43% modulation), this GRS 1915+105 and Cyg X-1, Her X-1, Sco X-1, and the Crab nebula object is likely a background AGN rather than a Galactic pulsar. The and pulsar. The long duration balloon flight will target several spectrum of the NuSTAR nebula shows evidence of an emission X-ray binaries and the extragalactic mass accreting supermassive line at E = 5.6 keV suggesting an optically obscured galaxy cluster black hole Cen A. In this contribution we give an update on the at z = 0.19+/-0.02 (d = 800 Mpc) and Lx = 1.2E44 erg/s. Follow-up status of the mission, and the expected science return. Chandra observations of Sh2-104 will help identify the nature of the X-ray sources and their relation to MGRO J2019+37. Author(s): Henric Krawczynski4, Fabian Kislat4 , David Stuchlik32 , Takashi Okajima , Gianluigi de Geronimo 1Author(s): Eric V. Gotthelf1 Institution(s): 1. Brookhaven National Laboratory, 2. Goddard Institution(s): 1. Columbia Astrophysics Lab. Space Flight Center, 3. Wallops Flight Facility, 4. Washington University in Saint Louis 117.02 – A Deep X-ray look at a very massive star: HETGS spectroscopy of the blue hypergiant Cyg 116.21 – Probing Sites of Extreme Astrophysics: the OB2-12 (HIP 101364) Science of ComPair We have obtained a Chandra/HETGS spectrum of one of the most Fundamental astrophysics questions ranging from characterizing massive and luminous stars in the Galaxy: the blue hypergiant Cyg the formation, structure, and properties of astrophysical jets and OB2-12 (HIP 101364, spectral type B3 Ia+). This is the first compact objects to explaining a large population of unidentified measurement at high resolution of X-ray spectral lines in a blue sources found by the Fermi Large Area Telescope can be addressed hypergiant and allows comparison of X-ray properties between by a mission that opens a window into the MeV range. ComPair massive stars at different but related evolutionary stages: O-type aims to provide excellent continuum sensitivity and good angular supergiants, luminous blue variables, Wolf-Rayet stars, and blue resolution over a wide field-of-view in the underexplored region hypergiants stars. The new data provide a look at how the most from ~200 keV to ~ 500 MeV. This critical band contains the massive stars shed mass during their pre-supernova evolution. We onset, peak, or fall of a rich variety of nonthermal processes find that In Cyg OB2-12 the resolved Si and Mg lines are broadened occurring at sites of strong gravitational and magnetic fields. by about 1000 km/s (FWHM). The lines, however, do not show ComPair will answer existing questions about well established appreciable centroid shifts (<100 km/s), which would be much source classes, such as MeV blazars, young luminous pulsars, and larger for canonical moderately thick winds (~500 km/s). The gamma-ray bursts, which are known to peak in energy flux within He-like Mg XI lines show evidence of photo-excitation, implying a wind origin close to the UV-bright photosphere. The spectrum also methods for various collisional velocities. Collisions of bare and indicates relatively high temperature plasma, up to 22 MK (1.9 H-like C to Al ions with H, He, and H2 are considered. Using these keV), showing significant continuum and emission lines below 5A line ratios, XSPEC models of CX emission in the northeast rim of (above 2.5 keV). Hence, at first glance, the spectrum resembles the Cygnus Loop supernova remnant will be shown as an example neither an O-star thick wind, nor a magnetically confined with ion velocity dependence. (narrow-line) plasma. We will present more detailed wind models using both X-ray and UV spectra to constrain fundamental physical [1] Henley, D. B. & Shelton, R. L. 2010, ApJSS, 187, 388 parameters of this star. [2] Dennerl, K. et al. 2002, A&A 386, 319 [3] Katsuda, S. et al. 2011, ApJ 730 24 Author(s): David Huenemoerder2, Lidia Oskinova3 , Richard [4] Cumbee, R. S. et al. 2014, ApJ 787 L31 Ignace132 , Wolf-Rainer Hamann , Norbert S. Schulz , hilding neilson43 , Tomer Shenar Author(s): Renata Cumbee1, David Lyons11 , Patrick Mullen , Institution(s): 1. East Tennessee State University, 2. MIT Kavli Robin L. Shelton112 , Phillip C. Stancil , David R. Schultz Institute, 3. University of Potsdam, 4. University of Toronto Institution(s): 1. University of Georgia, 2. University of North Texas 117.03 – The Dynamo Clinical Trial The Dynamo Clinical Trial evaluates long-term stellar magnetic health through periodic X-ray examinations (by the Chandra 118 – Supernovae and Supernova Remnants Observatory). So far, there are only three subjects enrolled in the DTC: Alpha Centauri A (a solar-like G dwarf), Alpha Cen B (an Poster Session early K dwarf, more active than the Sun), and Alpha Canis Majoris 118.01 – Constraining the Turbulence Scale and A (Procyon, a mid-F subgiant similar in activity to the Sun). Of Mixing of a Crushed Pulsar Wind Nebula these, Procyon is a new candidate, so it is too early to judge how it will fare. Of the other two, Alpha Cen B has responded well, with a Pulsar wind nebulae (PWNe) are synchrotron-emitting nebulae steady magnetic heartbeat of about 8 years duration. The sickest of resulting from the interaction between pulsars' relativistic particle the bunch, Alpha Cen A, was in magnetic cardiac arrest during outflows and the ambient medium. The Snail PWN in supernova 2005-2010, but has begun responding to treatment in recent years, remnant G327.1-1.1 is a rare system that has recently been crushed and seems to be successfully cycling again, perhaps achieving a by supernova reverse shock. We carried out radio polarization new peak of magnetic health in the 2016 time frame. If this is the observations with the Australia Telescope Compact Array and case, it has been 20 years since A's last healthful peak, significantly found highly ordered magnetic field structure in the nebula. This longer than the middle-aged Sun's 11-year magnetic heartbeat, but result is surprising, given the turbulent environment expected from perhaps in line with Alpha Cen A's more senescent state (in terms hydrodynamical simulations. We developed a toymodel and of "relative evolutionary age," apparently an important driver of compared simple simulations with observations to constrain the activity). (By the way, don't miss the exciting movie of the Alpha characteristic turbulence scale in the PWN and the mixing with Cen stars' 20-year X-ray dance.) supernova ejecta. We estimate that the turbulence scale is about one-eighth to one-sixth of the nebula radius and a pulsar wind Author(s): Thomas R. Ayres1 filling factor of 50-75%. The latter implies substantial mixing of the Institution(s): 1. University of Colorado pulsar wind with the surrounding supernova ejecta.

117.04 – The 3-year Solar Wind Charge Exchange This work is supported by an ECS grant of the Hong Kong Government under HKU 709713P. The Australia Telescope is Campaign with Suzaku: preliminary results funded by the Commonwealth of Australia for operation as a We performed a 3-year monitoring campaign of the Solar Wind National Facility managed by CSIRO. Charge Exchange (SWCX) heliospheric emission with Suzaku. We targeted four nearby (~100 pc) high column density clouds that Author(s): Chi Yung Ng5, Y. K. Ma54 , Niccolo Bucciantini , absorb the X-ray contribution from distant sources so that the Patrick O. Slane123 , Bryan M. Gaensler , Tea Temim leftover signal has local origin (and is expected to be dominated by Institution(s): 1. CfA, 2. Dunlap Institute for Astronomy and SWCX). The targets have been selected for their position in the sky, Astrophysics, 3. GSFC, 4. INAF, 5. The University of Hong Kong in order to maximize the latitude and longitude range, to model how SWCX depends on the distribution of neutrals, and to follow 118.02 – Asymmetric Expansion of the Youngest the seasonal variations of the SWCX. Here we present the results Galactic Supernova Remnant G1.9+0.3 of data analysis of the three years of observations and we show how they compare with existing models. The youngest Galactic supernova remnant (SNR) G1.9+0.3, produced by a (likely) Type Ia SN that exploded around CE 1900, is Author(s): Eugenio Ursino3, Massimiliano Galeazzi3 , Wenhao strongly asymmetric at radio wavelengths but exhibits a bilaterally Liu321 , Dimitra Koutroumpa , K. D. Kuntz symmetric morphology in X-rays. It has been difficult to Institution(s): 1. Johns Hopkins University, 2. LATMOS- understand the origin of these contrasting morphologies. We IPSL/CNRS, 3. University of Miami present results of X-ray expansion measurements of G1.9+0.3 that illuminate the origin of the radio asymmetry. These measurements 117.05 – The velocity dependence of X-ray emission are based on comparing recent (2015), 400 ks-long Chandra observations with earlier Chandra observations that include 1 due to Charge Exchange: Applications in the Cygnus Ms-long 2011 observations. The mean expansion rate from 2011 to Loop 2015 is 0.58% yr-1 , in agreement with previous measurements. We The fundamental collisional process of charge exchange (CX) has also confirm that expansion decreases radially away from the been been established as a primary source of X-ray emission from remnant's center along the major E-W axis, from 0.77% yr-1 to the heliosphere [1], planetary exospheres [2], and supernova 0.53% yr-1 . Large variations in expansion are also present along remnants [3,4]. In this process, X-ray emission results from the the minor N-S axis. Expansion of the faint S rim and the outermost capture of an electron by a highly charged ion from a neutral atom faint N rim is comparable to the mean expansion. But the or molecule, to form a highly-excited, high charge state ion. As the prominent X-ray rim in the N, coincident with the outer edge of the captured electron cascades down to the lowest energy level, bright radio rim that marks the primary blast wave there, is photons are emitted, including X-rays. expanding more slowly. Its expansion relative to the S rim is only To provide reliable CX-induced X-ray spectral models to 0.47% yr-1 . At 8.5 kpc, this corresponds to a speed of about 5000 realistically simulate high-energy astrophysical environments, line km/s, less than half of the overall blast wave speed of 12,000 km/s. ratios and spectra are computed using theoretical CX cross- Such strong deceleration of the northern blast wave most likely sections obtained with the multi-channel Landau-Zener, atomic- arises from the collision of SN ejecta with a much denser than orbital close-coupling, and classical-trajectory Monte Carlo average ambient medium there. The presence of the asymmetric ambient medium naturally explains the radio asymmetry. The SN developmental stages in detail, providing insight into stellar ejecta have also been strongly decelerated in the N, but they evolution, the mechanisms of the supernova explosion, and the expand faster than the blast wave. In several locations, significant transition from supernova to supernova remnant as the debris morphological changes and strongly nonradial motions are begins to interact with the surrounding circumstellar medium apparent. The spatially-integrated X-ray flux continues to increase (CSM). We present the latest results from 16 years of Chandra with time. As with Kepler's SN - the most recent historical SN in the ACIS observations of SN 1987A, now covering 4600 - 10500 days Galaxy - the SN ejecta are likely colliding with the asymmetric after the supernova. At approximately day 7500, the east-west circumstellar medium (CSM) ejected by the SN progenitor prior to asymmetry of the ring began to reverse, while the spectra and soft its explosion. G1.9+0.3 fills the gap between distant Type Ia-CSM X-ray light curve revealed that the increase in soft X-ray emission SNe and older Type Ia-CSM SNRs such as Kepler's SNR, providing slowed dramatically. This suggests the average CSM density us with a unique opportunity to learn about mysterious Type Ia encountered by the blast wave decreased at this time, likely due to progenitors. lack of new emission from the densest clumps in the equatorial ring. Since day 9700 the soft X-ray light curve has flattened and Author(s): Kazimierz J. Borkowski3, David Green1 , Peter remained approximately constant, evidence that the blast wave has Gwynne34 , Una Hwang , Robert Petre 2 , Stephen P. Reynolds 3 , now left the dense material of the known equatorial ring and is Rebecca Willett5 beginning to probe the unknown territory beyond. Institution(s): 1. Cavendish Laboratory, 2. NASA/Goiddard Space Flight Center, 3. North Carolina State Univ., 4. University of Author(s): Kari A. Frank1, David N. Burrows1 Maryland, 5. University of Wisconsin-Madison Institution(s): 1. Pennsylvania State University

118.03 – Spatially resolved spectroscopy analysis of 118.06 – The X-ray and Radio Evolution of SN 2005kd the XMM-Newton large program on SN1006 SN 2005kd is among the most luminous supernovae (SNe) to be We perform analysis of the XMM-Newton large program on discovered, at both X-ray and optical wavelengths. We have SN1006 based on our newly developed methods of spatially re-analysed all good angular resolution archival X-ray data resolved spectroscopy analysis. We extract spectra from low and available for SN 2005kd, combined with a 29ks Chandra high resolution meshes. The former (3596 meshes) is used to observation obtained by our group. The data reveal an X-ray light roughly decompose the thermal and non-thermal components and curve that decreases faster than is expected for expansion in a characterize the spatial distributions of different parameters, such steady wind. Our modelling of the data suggests that the early as temperature, abundances of different elements, ionization age, evolution is dominated by emission from the forward shock in a and electron density of the thermal component, as well as photon high-density medium. The observations suggest that the SN is index and cutoff frequency of the non-thermal component. On the expanding into a high density and high mass-loss rate other hand, the low resolution meshes (583 meshes) focus on the environment, which is also supported by our analysis of the interior region dominated by the thermal emission and have available radio data. Our results are used to estimate the mass-loss enough counts to well characterize the Si lines. We fit the spectra rate of the progenitor, variability in the wind mass-loss parameters from the low resolution meshes with different models, in order to prior to core-collapse, and the nature of the progenitor. decompose the multiple plasma components at different thermal and ionization states and compare their spatial distributions. In Author(s): Vikram Dwarkadas2, Cristina Romero-Canizales1 , this poster, we will present the initial results of this project. Ratuja Reddy21 , Franz E. Bauer Institution(s): 1. Millennium Institute of Astrophysics, 2. Univ. Author(s): Jiang-Tao Li5, Anne Decourchelle13 , Marco Miceli , of Chicago Jacco Vink42 , Fabrizio Bocchino Institution(s): 1. CEA Saclay, 2. INAF-Osservatorio 118.07 – Investigating the X-ray Emission from some Astronomico di Palermo, 3. Universita di Palermo, 4. University of of the Oldest Known X-ray Supernovae Amsterdam, 5. University of Michigan The core-collapse of a massive star results in a supernova (SN) explosion, and a shock wave that expands outwards. The evolution 118.04 – Smoothed Particle Inference Analysis of SNR of the shock wave, and the radius and morphology of the resulting RCW 103 remnant, depends on the density structure of the SN ejecta and We present preliminary results of applying a novel analysis surrounding medium. As the SN evolves, it sweeps up more method, Smoothed Particle Inference (SPI), to an XMM-Newton material. The shock velocity, and therefore post-shock temperature observation of SNR RCW 103. SPI is a Bayesian modeling process (proportional to the square of the shock velocity), will that fits a population of gas blobs ("smoothed particles") such that consequently decrease. Thus we would expect a gradual evolution their superposed emission reproduces the observed spatial and in the X-ray properties of the SN. While theoretical models spectral distribution of photons. Emission-weighted distributions anticipate this, very few SNe have observations over several of plasma properties, such as abundances and temperatures, are decades that allow us to probe the time evolution of the X-ray then extracted from the properties of the individual blobs. This emission and SN shocks. technique has important advantages over analysis techniques which implicitly assume that remnants are two-dimensional We have compiled a database of most observed X-ray SNe. In this objects in which each line of sight encompasses a single plasma. By talk we will summarize the X-ray data on some of the oldest contrast, SPI allows superposition of as many blobs of plasma as detected X-ray SNe. These observations bridge the gap between old are needed to match the spectrum observed in each direction, SNe and young supernova remnants, and shed light on the without the need to bin the data spatially. This RCW 103 analysis is transition of a supernova to a remnant. We will show lightcurves part of a pilot study for the larger SPIES (Smoothed Particle for those which have multiple detections, outline the variation in Inference Exploration of SNRs) project, in which SPI will be their X-ray luminosity with time, compare their X-ray emission to applied to a sample of 12 bright SNRs. that of younger supernovae, and discuss the evolution of the shock parameters as the supernova continues on its journey towards Author(s): Kari A. Frank1, David N. Burrows1 , Vikram becoming a remnant. Dwarkadas2 Institution(s): 1. Pennsylvania State University, 2. University of Author(s): Vikram Dwarkadas1, Danika Holmes1 Chicago Institution(s): 1. Univ. of Chicago

118.05 – SN 1987A: Chandra Witnesses the End of an 118.08 – X-ray Properties of Supernova Remnants in Era Nearby Spiral Galaxies Due to its age and close proximity, the remnant of SN 1987A is the More extragalactic SNRs have been detected in X-rays in nearby only supernova remnant in which we can study the early galaxies than in the Milky Way. Most of the X-ray detected SNRs were first identified optically, and then detected as soft X-ray insight into the density structure, composition and metallicity of sources in deep imaging observations with Chandra and in some the surrounding medium, and the ionization level, through the cases XMM. Here, we discuss the large X-ray samples of SNRs in spectra themselves as well as the X-ray absorption. M33, M51, M83, and M101, with the goal of understanding which SNRs are detected in X-rays and which are not. Not surprisingly In this presentation we will show the lightcurves of almost all IIns perhaps, most of the SNRs in these galaxies are middle-aged ones that have been observed in the X-ray band, and compare and very few analogs of Cas A, the Crab or other young objects have contrast them to the X-ray lightcurves of other types of SNe. We been found. Trends of X-ray luminosity with diameter are absent, summarize the known properties of the X-ray emission from Type probably because the total amount of swept up material is the IIn SNe, and explore the implications for the SN environment, dominant factor in determining the X-ray luminosity of a SNR at a progenitor mass-loss and the identity of the progenitors. particular time. SNRs expanding into high density media evolve rapidly and have X-ray luminosities that peak at small diameters, Author(s): Vikram Dwarkadas1 whereas those expanding into lower density media evolve more Institution(s): 1. Univ. of Chicago slowly and have luminosities that peak later. 118.11 – G156.2+5.7: SN 1006's older cousin Author(s): Knox S. Long3, William P. Blair11 , K. D. Kuntz , P. We report on the results of an analysis of the hydrodynamic Frank Winkler2 properties of the supernova remnant G156.2+5.7. The models of Institution(s): 1. JHU, 2. Middlebury College, 3. STScI Truelove and McKee (1999) are constrained by the observed amount of thermal X-ray emission, the measured temperature of 118.09 – The Variable Crab Nebula: Evidence for a the forward-shocked electrons, the inferred location of the reverse Connection between GeV flares and Hard X-ray shock, and the observed amount of non-radiative Balmer line Variations emission. The results suggest that the remnant is expanding into a In 2010, hard X-ray variations (Wilson-Hodge et al. 2011) and GeV low-density environment at a distance of at least 0.6 kpc. We flares (Tavani et al 2011, Abdo et al. 2011) from the Crab Nebula review several clues that suggest the remnant was produced by a were discovered. Connections between these two phenomena were Type Ia supernova, which when combined with the other unclear, in part because the timescales were quite different, with hydrodynamic constraints, implies that G156.2+5.7 is 2.6-15 kyr yearly variations in hard X-rays and hourly to daily variations in the old, is 0.7-1.7 kpc from Earth (i.e. between Earth and the Perseus GeV flares. The hard X-ray flux from the Crab Nebula has again arm), and is surrounded by material with a hydrogen density of declined since 2014, much like it did in 2008-2010. During both 0.046-0.075 cm-3 . These properties are consistent with the hard X-ray decline periods, the Fermi LAT detected no GeV flares, remnant having a low radio surface brightness with a highly- suggesting that injection of particles from the GeV flares produces ordered and highly-polarized, tangential magnetic field that is the much slower and weaker hard X-ray variations. The timescale inclined by 60-70 degrees relative to the Galactic plane. However, for the particles emitting the GeV flares to lose enough energy to the inferred density and age are not consistent with the fitted value emit synchrotron photons in hard X-rays is consistent with the of the ionization age, which may indicate that the momentum yearly variations observed in hard X-rays and with the expectation distribution of the electrons is not a Maxwell-Boltzmann that the timescale for variations slowly increases with decreasing distribution, but instead includes a high-energy, non-thermal tail. energy. This hypothesis also predicts even slower and weaker variations below 10 keV, consistent with the non-detection of Author(s): Glenn E. Allen2, Thomas Pannuti3 , Allana counterparts to the GeV flares by Chandra (Weisskopf et al 2013). Iwanicki14 , William Tan We will present a comparison of the observed hard X-ray variations Institution(s): 1. Milton Academy, 2. MIT, 3. Morehead State and a simple model of the decay of particles from the GeV flares to University, 4. Northeastern test our hypothesis. 118.12 – Radio Observations of the Pulsar Wind Author(s): Colleen A. Wilson-Hodge5, Alice Kust Harding4 , Nebula HESS J1303−631 with ATCA Elizabeth A. Hays421 , Michael L. Cherry , Gary L. Case , Mark H. Based on its enregy-dependent morphology the initially Finger76 , Peter Jenke , Xiao-Ling Zhang 3 unidentified very high energy (VHE; E > 100 GeV) gamma-ray Institution(s): 1. La Sierra University, 2. LSU, 3. MPE, 4. source HESS J1303−631 was recently associated with the pulsar NASA/GSFC, 5. NASA/MSFC, 6. UAH, 7. USRA/MSFC PSR J1301−6305. Subsequent detection of X-ray and GeV counterparts further supports the identification of the H.E.S.S. 118.10 – The X-ray emission from Type IIn Supernovae source as evolved pulsar wind nebula (PWN). Recent radio as a Probe of the Stellar Environment and Supernova observations of the PSR J1301−6305 region with ATCA dedicated Progenitors to search for the radio counterpart of HESS J1303-631 are reported Core-collapse supernovae (SNe) are divided into different here. Observations at 5.5 GHz and 7.5 GHz do not reveal any subclasses, depending mainly on their optical spectra or light curve. extended emission associated with the pulsar. The analysis of the Type IIn supernovae (SNe) form one of the more recent archival 1.384 GHz and 2.368 GHz data also does not show any subclasses, having been first identified in 1990. They are significant emission. The 1.384 GHz data reveal a hint of an characterized by narrow lines on a broad base in the optical extended shell-like emission in the same region which might be a spectrum, and comprise 1 to 4% of the total core collapse SN supernova remnant. The implications of the non-detection at radio population. There exists a wide diversity in SNe that exhibit IIn wavelengths on the nature and evolution of the PWN as well as the features, which has greatly complicated the task of identifying their possibility of the SNR candidate being a birth place of PSR progenitors. J1301−6305 are discussed. 5 34 IIns are observed to have the highest X-ray luminosity of all the SN Author(s): Iurii Sushch , Igor Oya , Ullrich Schwanke , 21 classes, with luminosities generally exceeding 1038 ergs/s after Simon Johnston , Matthew Dalton several thousand days. Thus they are observable in X-rays even at Institution(s): 1. Active Space Technologies GmbH, 2. Australia late times, hundreds to thousands of days after explosion. They Telescope National Facility, 3. DESY Zeuthen, 4. Humboldt also exhibit the most diversity in their light curves. Many of the University of Berlin, 5. North-West University lightcurves tend to fall off rather steeply at late times, although one interesting case displayed a rising light curve for several thousand days. These characteristics, along with their high luminosities at 119 – WDs & CVs Poster Session other wavelengths, imply initial expansion in a very dense medium, with the densities decreasing rapidly a few years after explosion. 119.01 – Astrophysical Boundary Layers: A New Their X-ray spectra generally show distinct lines, suggesting that Picture the emission is thermal in origin. The X-ray spectra can provide Accretion is a ubiquitous process in astrophysics. In cases when the magnetic field is not too strong and a disk is formed, accretion can difference primarily in the different ages and metallicity of the proceed through the mid plane all the way to the surface of the HMXB populations in the two galaxies. We also set limits on the central compact object. Unless that compact object is a black hole, a kicks imparted on the neutron star during the supernova boundary layer will be formed where the accretion disk touches its explosion. We find that the time elapsed since the supernova kick surfaces. The boundary layer is both dynamically and is ∼3 times shorter in the LMC than the SMC. This in combination observationally significant as up to half of the accretion energy is with the average offsets of the HMXBs from their nearest star dissipated there. clusters results in ∼4 times faster transverse velocities for HMXBs Using a combination of analytical theory and computer simulations in the LMC than in the SMC. we show that angular momentum transport and accretion in the boundary layer is mediated by waves. This breaks with the standard Author(s): Vallia Antoniou1, Andreas Zezas1 astrophysical paradigm of an anomalous turbulent viscosity that Institution(s): 1. Smithsonian Astrophysical Observatory drives accretion. However, wave-mediated angular momentum transport is a natural consequence of "sonic instability." The sonic 120.03 – NuSTAR discovers a cyclotron line and instability, which we describe analytically and observe in our reveals the spinning up of the accreting X-ray pulsar simulations, is a close cousin of the Papaloizou-Pringle instability. IGR J16393-4643 However, it is very vigorous in the boundary layer due to the After several misclassifications, IGR J16393-4643 is now known to immense radial velocity shear present at the equator. be a high-mass X-ray binary consisting of a heavily-absorbed Our results are applicable to accreting neutron stars, white dwarfs, pulsar that is likely paired with a massive and distant B star. It was protostars, and protoplanets. observed for 50-ks by NuSTAR in the 3--79 keV energy band, complemented by a contemporaneous 2-ks observation with Author(s): Mikhail Belyaev3, Roman R. Rafikov1 , James 2 Swift-XRT. These observations enabled the discovery of a cyclotron Mclellan Stone resonant scattering feature with a centroid energy of Institution(s): 1. Institute for Advanced Study, 2. Princeton 29.3(+1.1/-1.3) keV. This allowed us to measure the magnetic field University, 3. UC Berkeley strength of the neutron star for the first time: B = (2.5±0.1)×1012 G. The known pulsation period is now observed at 904.0±0.1 s. Since 2006, the neutron star has undergone a long-term spin-up 120 – XRBs and Population Surveys Poster trend at a rate of dP/dt = -2×10-8 s s -1 (-0.6 s per year, or a Session frequency derivative of dν/dt = 3×10-14 Hz s -1 ). In the power density spectrum, a break appears at the pulse frequency which 120.01 – The Ionized and Variable Outflow in the separates the zero slope at low frequency from the steeper slope at Low-Mass X-Ray Binary GX 13+1 high frequency. This addition of angular momentum to the We present the analysis of 7 Chandra HETG and 16 simultaneous neutron star could be due to the accretion of a quasi-spherical RXTE PCA observations of GX 13+1, a persistent neutron star wind, or it could be caused by the transient appearance of a prograde accretion disk that is nearly in corotation with the low-mass X-ray binary. The observations cover activity between 8 2002 and 2011. The 0.5-10 keV continuum was consistent with a neutron star whose magnetospheric radius is around 2×10 cm. two component model, either a blackbody plus power law or Author(s): Arash Bodaghee5, John Tomsick10 , Francesca multicolor disk and blackbody across luminosities of (5-7)x1037 Fornasini10 , Roman Krivonos 9 , Daniel Stern 6 , Kaya Mori 2 , Farid erg sec-1 , modified by a neutral absorption column requiring a Rahoui4103 , Steven E. Boggs , Finn Christensen , William W. silicon overabundance. We have identified significantly Craig7218 , Charles James Hailey , Fiona Harrison , William Zhang blue-shifted (v > 500 km sec-1 ) Kα Fe, Ca, S, and Si outflow Institution(s): 1. Caltech, 2. Columbia University, 3. Danish hydrogen-like lines in all HETG observations, as well Technical University, 4. European Southern Observatory, 5. hydrogen-like Ar and Mg lines in the majority of observations. The Georgia College and State University, 6. JPL-Caltech, 7. Lawrence significant outflow can be modeled as a photoionized plasma with Livermore National Laboratory, 8. NASA's GSFC, 9. Space an ionization parameter ≥ 3.5. For the first time we map the Research Institute (IKI), 10. University of California, Berkeley occurrence of these wind outflows onto the color-color diagram of GX 13+1 and compare their location with that of the jet outflows in this system. We will further present variable X-ray properties of the 120.04 – Multiwavelength Studies of Transitional wind in GX 13+1 and discuss suggested launching mechanisms as Millisecond Pulsars well as how its properties relate to the wind-accretion state in The recent discovery of three millisecond pulsar (MSP) binary low-mass X-ray binaries. systems that alternate between clearly distinguishable rotation- and accretion-powered states have revealed a new aspect of Author(s): Jessamyn Allen1, Norbert S. Schulz2 , Jeroen compact binaries containing neutron stars. These so-called Homan21 , Deepto Chakrabarty transitional MSP systems hold the promise to elucidate the poorly- Institution(s): 1. Department of Physics, MIT, 2. Kavli Institute understood transition mechanism of pulsars between accretion and for Astrophysics & Space Research, MIT rotation power, as well as the detailed physics of accretion onto magnetized objects and the attendant outflows/jets. In this talk, I 120.02 – The formation efficiency of high-mass X-ray will present the rich phenomenology of transitional MSPs as binaries in our two nearest star-forming galaxies revealed by our on-going X-ray, optical, and radio observing We present the results of our investigation of the link between campaigns and discuss prospects for expanding the sample of these high-mass X-ray binaries (HMXBs) and star formation in the objects using the forthcoming Neutron Star Interior Composition Magellanic Clouds, our nearest star-forming galaxies. Using the Explorer X-ray timing instrument. most complete census of HMXBs in the Large Magellanic Cloud Author(s): Slavko Bogdanov2, Anne M Archibald1 , Cees (LMC) and the published spatially resolved star-formation history Bassa111 , Adam T Deller , Jason Hessels , Jules P. Halpern 2 , map of this galaxy, we find that the HMXBs (and as expected the Amruta Jaodand1 X-ray pulsars) are present in regions with star-formation bursts Institution(s): 1. ASTRON, 2. Columbia University ∼6-25 Myr ago. In contrast, this population peaks at later ages (∼25-60 Myr ago) in the Small Magellanic Cloud (SMC). Thus, this study (in combination with previous works) reinforces the idea that 120.05 – Enhanced X-ray Emission from Early the HMXBs are associated with young stellar populations of ages Universe Analog Galaxies ∼10-40 Myr. In addition, we estimate an HMXB production rate of X-rays from binaries containing compact objects may have played 1 system per ∼(23.0-4.1+4.4) ×10 -3 M⊙/yr or 1 system per an important role in heating the early Universe. Here we discuss ∼143M⊙ of stars formed during the associated star-formation our findings from X-ray studies of blue compact dwarf galaxies episode. Therefore, the formation efficiency of HMXBs in the LMC (BCDs), Lyman break analogs (LBAs), and Green Pea galaxies is ∼17 times lower than that in the SMC. We attribute this (GP), all of which are considered local analogs to high redshift galaxies. We find enhanced X-ray emission per unit star-formation wavelength analysis of 1FGL J1018.6-5856 with the Australia rate which strongly correlates with decreasing metallicity. We find Telescope Compact Array (ATCA), Fermi LAT and the Swift X-ray evidence for the existence of a L_X-SFR-Metallicity plane for Telescope (XRT) to better determine the properties of the star-forming galaxies. The exact properties of X-ray emission in the 16.531$\pm$0.006 day orbital modulation. The radio amplitude early Universe affects the timing and morphology of reionization, modulation is found to decline with increasing frequency, which is both being observable properties of current and future radio a possible indication of the presence of free-free absorption. This is observations of the redshifted 21cm signal from neutral hydrogen. further supported by the absence of clear modulation in the 33.0 and 35.0\,GHz bands, which were not previously reported. The Author(s): Matthew Brorby4, Philip Kaaret4 , Andrea H. best-fit spectral model of the Swift XRT data consists of a Prestwich213 , I. Felix Mirabel , Hua Feng featureless power law with index $\Gamma\sim$1.3--1.7 modified Institution(s): 1. CEA-CEN Saclay, 2. Harvard-Smithsonian by an absorber that fully covers the source. This is possible CfA, 3. Tsinghua University, 4. University of Iowa evidence that 1FGL J1018.6-5856 is a non-accreting system.

120.06 – An Investigation of Luminous X-Ray Pulsars: Author(s): Joel Barry Coley2, Robin Corbet53 , Chi C. Cheung , Exploring Accretion Onto Magnetized the Neutron Guillaume Dubus41 , Philip Edwards , Vanessa McBride 6 , Jamie Star LMC X-4 Stevens1 X-ray pulsars are neutron stars in which magnetic forces dominate Institution(s): 1. CSIRO Astronomy and Space Science, 2. NASA accretion within the magnetosphere. These systems offer unique Goddard Space Flight Center, 3. Naval Research Laboratory, 4. laboratories to study magnetic accretion and the behavior of matter UJF-Grenoble, 5. UMBC, 6. University of Cape Town under extreme densities, magnetic fields, and gravitational forces. Using joint observations with NuSTAR and XMM-Newton, we 120.09 – The broadband spectrum of Centaurus X-3 observe the complete precession of the warped accretion disk We present an analysis of a Suzaku observation of the accreting around the X-ray pulsar LMC X-4, and measure the relative phase pulsar and high mass X-ray binary Centaurus X-3. The observation between the pulsar beam and the softer X-ray photons reprocessed was performed in 2008 and covers one 2.1 day binary orbit. Strong by the disk. This allows us to perform tomography to explore the flux and hardness variability is present in the energy range from inner magnetized accretion flow. Additionally, we investigate the 0.8 to 60 keV. We selected a part of the observation covering ~40% unusual flaring events observed from LMC X-4 during October and of the first half of the orbit during which the spectral shape was November of 2015. stable and less absorbed than during other parts of the observation. We confirm earlier results that the broadband spectrum can be Author(s): McKinley Brumback1 modeled with a Institution(s): 1. Dartmouth College cutoff power law modified by a partial absorber, three iron lines -- from near-neutral, helium-like, and hydrogen-like iron --, and a 120.07 – A test of the nature of the Fe K Line in the cyclotron resonant scattering line at 30 keV. The pulse profile neutron star low-mass X-ray binary Serpens X-1 shows a shift above the cyclotron line energy which is qualitatively Broad Fe K emission lines have been widely observed in the X-ray consistent with recent theoretical predictions. In addition we find spectra of black hole systems, and in neutron star systems as well. that the presence of the so-called ``13 keV'' bump is model The intrinsically narrow Fe K fluorescent line is generally believed dependent and that there are indications for further line-like to be part of the reflection spectrum originating in an illuminated spectral components at 1 keV and 6 keV and a broader residual accretion disk, and broadened by strong relativistic effects. around 2 keV. We also apply the newly implemented radiation However, the nature of the lines in neutron star LMXBs has been dominated radiative shock model for luminous accretion pulsars by under debate. We therefore obtained the longest, high-resolution Becker and Wolff (2007, ApJ 654, 435) to model the broadband X-ray spectrum of a neutron star LMXB to date with a 300 ks spectrum. Replacing the cutoff power law with the physical Chandra HETGS observation of Serpens X-1. The observation was continuum while retaining all other components we obtain a taken under the "continuous clocking" mode and thus free of similar goodness of fit as before. From the physical continuum photon pile-up effects. We carry out a systematic analysis and find model we determine a mass accretion rate of ~2.17 x 10^17 g/s, an that the blurred reflection model fits the Fe line of Serpens X-1 accretion column radius of 65 (+12, -4) m, and a temperature of the significantly better than a broad Gaussian component does, accreted plasma of 3.1 (+0.4, -0.1) keV. implying that the relativistic reflection scenario is much preferred. Author(s): Amy Gottlieb6, Katja Pottschmidt33 , Diana Marcu , Chandra HETGS also provides highest spectral resolution view of Michael Thomas Wolff41 , Matthias Kühnel , Sebastian Falkner 1 , the Fe K region and we find no strong evidence for additional Paul Britton Hemphill552 , Slawomir Suchy , Peter A. Becker , Kent narrow lines. S. Wood41 , Joern Wilms Author(s): Chia-Ying Chiang12, Edward Cackett12 , Jon M. Institution(s): 1. Dr. Karl Remeis-Observatory & ECAP, Miller10 , Didier Barret 7 , Andrew C Fabian 8 , Antonino D'Ai 1 , University of Erlangen-Nuremberg, 2. George Mason University, Michael Parker845 , Sudip Bhattacharyya , Luciano Burderi , Tiziana 3. NASA Goddard Space Flight Center, 4. Naval Research Salvo62 , Elise Egron , Jeroen Homan 3 , Rosario Iaria 6 , Dacheng Laboratory, 5. University of California, San Diego, 6. University of Lin11 , M. Coleman Miller 9 Florida Institution(s): 1. INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, 2. INAF-Osservatorio Astronomico di 120.10 – Driving of Accretion Disk Variability by the Cagliari, 3. MIT, 4. Tata Institute of Fundamental Research, 5. Disk Dynamo Universita degli Studi di Cagliari, 6. Universita di Palermo, 7. Variability is a ubiquitous feature of emission from accreting Universite de Toulouse, 8. University of Cambridge, 9. University objects, but many questions remain as to how the variability is of Maryland, 10. University of Michigan, 11. University of New driven and how it relates to the underlying accretion physics. In Hampshire, 12. Wayne State University this talk I will discuss recent results from a long, semi-global MHD simulation of a thin accretion disk around a black hole used to 120.08 – A Multi-Wavelength Study of the Gamma-Ray perform a detailed study of the fluctuations in the internal disk Binary 1FGL J1018.6-5856 stress and the influence these fluctuations have on the accretion 1FGL J1018.6-5856, the first gamma-ray binary discovered by the flow. In the simulation, low frequency fluctuations of the effective Fermi Large Area Telescope (LAT), consists of an O6 V((f)) star and α-parameter in the disk are linked to oscillations of the disk suspected rapidly spinning pulsar. While 1FGL J1018.6-5856 has dynamo. These fluctuations in the effective alpha parameter drive been postulated to be powered by the interaction between a “propagating fluctuations” in mass accretion rate through the disk relativistic pulsar wind and the stellar wind of the companion, a that qualitatively resemble the variability from astrophysical black microquasar scenario where the compact object is a black hole hole systems. The mass accretion rate has several of the ubiquitous cannot be ruled out. We present the first extensive multi- phenomenological properties of black hole variability, including log-normal flux distributions, RMS-flux relationships, and radial rotate around the star at the star's spin frequency. We first discuss coherence. the phenomenology and modeling of these oscillations. We then present the results of parameter estimation studies using synthetic Author(s): J. Drew Hogg1, Christopher S. Reynolds1 waveform data and Bayesian statistical methods. The synthetic and Institution(s): 1. University of Maryland model waveforms used in this study were computed using the X-ray spectra and radiation beaming patterns given by models of 120.11 – X-Ray Reflection of Thermonuclear Bursts the cool hydrogen atmospheres that NICER is expected to observe. from Neutron Stars: Constraining Flames with RXTE Finally, we discuss the causes and expected sizes of the and an Outlook on NICER uncertainties in radius and mass estimates that will be made by Thermonuclear X-ray bursts observed from accreting neutron stars NICER using this method. are employed to study, e.g., the nuclear physics of rare isotopes and 1 2 the dense matter equation of state. Recent observations indicate Author(s): Frederick K. Lamb , M. Coleman Miller that bursts strongly affect their accretion environment, and Institution(s): 1. Univ. of Illinois, 2. Univ. of Maryland reprocessed burst emission may reflect off the inner accretion disk. The spectra of the short (10-100s) bursts are, however, of 120.14 – NUSTAR AND XMM-Newton Observations of insufficient quality to accurately separate the neutron star signal the Neutron Star X-Ray Binary 1RXS J180408.9-34205 from accretion disk emission and burst reflection. Only for two rare We report on observations of the neutron star (NS) residing in the "superbursts" with durations of several hours did RXTE/PCA low-mass X-ray binary 1RXS J180408.9- spectra show burst reflection signatures. We discuss the case of 4U 34205 taken 2015 March by NuSTAR and XMM-Newton while the 1636-536, where the reflection signal traced the evolution of the source was in the hard spectral state. We find ionization state of the inner disk. Our simulations show that a large multiple reflection features (Fe Kα detected with NuSTAR; N VII, O reflection fraction may indicate that the disk puffs up due to burst VII, and O VIII detected in the RGS) from irradiation. After separating the direct burst emission from different ionization zones. Through joint fits using the self reflection, we show that the rise of the superburst light curve is consistent relativistic reflection model RELXILL, shaped by a stalling carbon flame. In the near future, the Neutron we determine the inner radius to be 6.6(+13.2,−0.6) Rg. We find Star Interior Composition ExploreR (NICER) will have a band-pass the inclination of the system to be between 18-29 degrees. that extends below 2 keV, where reflection dominates the burst If the disk is truncated at a radius greater than the innermost stable spectrum, and which was not probed by RXTE. Therefore, NICER circular orbit (ISCO), then the position at which the inner disk will be able to detect reflection features during the frequent short terminates likely corresponds to the magnetospheric radius. For a bursts. NICER will open a new field of studying the interaction of spin parameter of a = 0, we estimate a conservative upper limit on bursts and the accretion environment, which will inform us of the strength of the magnetic field to be B ≤ (0.9 − 3.0) × 109 G at which bursts are optimally suited for neutron star mass-radius the magnetic poles depending on the choice of conversion factor measurements. between spherical and disk accretion.

Author(s): Laurens Keek1 Author(s): Renee Ludlam7, Jon M. Miller78 , Edward Cackett , Institution(s): 1. University of Maryland/NASA GSFC Andrew C Fabian323 , Matteo Bachetti , Michael Parker , John Tomsick65 , Didier Barret , Lorenzo Natalucci 41 , Vikram Rana , 120.12 – The Recent Outburst of SMC X-2 as seen by Fiona Harrison1 Swift, MAXI and NuSTAR Institution(s): 1. California Institute of Technology, 2. We present results from the latest outburst of the Be/X-ray binary INAF/Osservatorio Astronomico di Cagliari, 3. Institute of system SMC X-2, which in late 2015 entered it's first X-ray Astronomy, 4. Istituto Nazionale di Astrofisica, 5. Universit de outburst since 2000. SMC X-2 was first discovered in 1977 by the Toulouse, 6. University of California, 7. University of Michigan, 8. SAS-3 satellite, and hosts a 2.37s period pulsar. Regular, almost Wayne State University daily, Swift observations of SMC X-2 were performed during the entirety of the latest outburst, from first detection by MAXI to it’s 120.15 – X-Ray Burst Oscillations: From Flame rapid turn off and return back to quiescence. These observations Spreading to the Cooling Wake have allowed us to measure with the flux, spectral and temporal Type I X-ray bursts are thermonuclear flashes observed from the properties of SMC X-2. Timing analysis of observation by the Swift surfaces of accreting neutron stars (NSs) in Low Mass X-ray X-ray telescope allowed us to track the evolution of the pulsar spin Binaries. Oscillations have been observed during the rise and/or period, and in addition modeling of the orbital parameters of the decay of some of these X-ray bursts. Those seen during the rise can system by measuring changes in the pulsar spin period due to be well explained by a spreading hot spot model, but large Doppler effects. In addition we report on an observation of SMC amplitude oscillations in the decay phase remain mysterious X-2 taken with NuSTAR, which allowed both to better measure the because of the absence of a clear-cut source of asymmetry. To date continuum fit above 10 keV, and to perform a sensitive measure of there have not been any quantitative studies that consistently track the pulse profile and period of the source. the oscillation amplitude both during the rise and decay (cooling tail) of bursts. In this talk I will discuss the results of our Author(s): Jamie Kennea2, Malcolm J. Coe34 , Silas Laycock , computations of the light curves and amplitudes of oscillations in Tony Bird366 , Elizabeth Bartlett , Lee Townsend , Vanessa X-ray burst models that realistically account for both flame McBride651 , Robin Corbet , Frank Haberl , Georgios Vasilopoulos 1spreading and subsequent cooling. I will present results for several Institution(s): 1. MPE, 2. Penn State, 3. Southampton such “cooling wake” models, a “canonical” cooling model where University, 4. UMass Lowell, 5. UMBC, 6. University of Cape each patch on the NS surface heats and cools identically, or with a Town latitude-dependent cooling timescale set by the local effective gravity, and an “asymmetric” model where parts of the star cool at 120.13 – Measuring neutron star masses and radii significantly different rates. We show that while the canonical using NICER observations of X-ray oscillations cooling models can generate oscillations in the tails of bursts, they Precise and reliable simultaneous measurements of the mass and cannot easily produce the highest observed modulation radius of several neutron stars with different masses would provide amplitudes. Alternatively, a simple phenomenological model with valuable guidance for improving models of the properties of cold asymmetric cooling can achieve higher amplitudes consistent with dense matter. The prime scientific goal of the Neutron star Interior the observations. I will discuss how the combination of the light Composition ExploreR (NICER) is to make such measurements by curve and fractional amplitude evolution can constrain the fitting energy-dependent waveform models to the thermal X-ray properties of the flame spreading, such as ignition latitude, the oscillations observed from rotation-powered millisecond pulsars. flame spreading geometry and speed, and its latitudinal These oscillations are thought to be produced as hotter regions of dependence which would be important for measuring NSs masses the stellar surface near one or both of the star’s magnetic poles and radii using X-ray burst oscillations. Author(s): Simin Mahmoodifar1, Tod E. Strohmayer1 orbit. We use the Chandra and XMM-Newton eclipse ephemeris Institution(s): 1. NASA/GSFC residuals to describe this third body orbit.

120.16 – Cygnus X-3 Little Friend's Counterpart, the Author(s): Michael Nowak2, Deepto Chakrabarty2 , Joern Distance to Cygnus X-3 and Jets (Oh My!) Wilms11 , Matthias Kühnel Institution(s): 1. Karl Remeis Observatory, 2. MIT Kavli Chandra observations have revealed a feature within 16" of Cygnus Institute X-3 which varied in phase with Cygnus X-3. This feature was shown to be a Bok globule which is along the line of sight to Cygnus X-3. We report on 120.19 – The XLF of LMXBs in the fields of early-type observations made with Submillimeter Array (SMA) to search for galaxies, their metal-rich, and metal-poor globular molecular emission from this globule, also known as Cygnus X-3's clusters "little friend." We have found a counterpart in both 12CO and 13CO The X-ray luminosity function (XLF) of extragalactic low mass emission. From the velocity shift of the molecular lines we are able X-ray binaries (LMXBs) can provide insights into their nature and determine a kinematic distance to the little friend and in turn a origin. We present an analysis of seven early-type galaxies. These distance to Cygnus X-3. The uncertainties in this distance estimate galaxies have deep Chandra observations, which detect X-ray to Cygnus X-3 are less than 10%. An additional unexpected sources down to 1037 erg/s, and HST optical mosaics that enable discovery was that Cygnus X-3 is not the only source to have jets! the classification of these sources into field LMXBs, globular cluster (GC) LMXBs, and contaminating sources. At all Author(s): Michael L. McCollough1, Michael M. Dunham1 , luminosities, we find that the number of field LMXBs per stellar Lia Corrales2 mass is similar in these galaxies. This sample therefore suggests Institution(s): 1. Harvard-Smithsonian, CfA, 2. MIT that the GC specific frequency may not influence the field LMXB population. It also suggests that other parameters, such as the 120.17 – The Case for PSR J1614-2230 as a NICER stellar IMF, are either similar across the galaxy sample or vary in a Target way that does not effect the LMXB population. The XLF of the field The Neutron star Interior Composition ExploreR (NICER) will and GC LMXBs are significantly different (p-value of 3x10-6 ), with launch in 2016 and will spend two years gathering X-ray data on the latter having a flatter XLF. The XLFs of the metal-rich and neutron stars and other high-energy sources from a berth on the metal-poor GC LMXBs are similar, although larger samples will be International Space Station. Its prime scientific goal is to measure needed to provide sharper tests in the future. the masses and radii of non-accreting neutron stars via fits to the 1 1 energy-dependent waveforms produced by the rotation of hot spots Author(s): Mark Peacock , Steve E. Zepf on their surfaces. These measurements will provide valuable input Institution(s): 1. Michigan State University to theoretical models of cold matter beyond nuclear density. Here we propose that PSR J1614-2230, despite its low count rate, is a 120.20 – The Swift Supergiant Fast X-ray Transients promising source to observe with NICER. The reason is that outburst factory XMM-Newton observations suggest that the fractional oscillation We present the Swift Supergiant Fast X-ray Transients project, amplitude from PSR J1614-2230 could be high enough that this which has been exploiting Swift's capabilities in a systematic study star cannot be very compact. We show that if we can analyze 0.5 of SFXTs and classical supergiant X-ray binaries (SGXBs) since Msec of NICER data and 0.1 Msec of nearby off-source data, and 2007. We performed an efficient long-term monitoring of 16 combine that analysis with the known mass of this star, we would sources including both SFXTs and classical SGXBs and followed find a robust lower limit to the radius with a statistical uncertainty source activity across more than 4 orders of magnitude in X-ray of only 0.5-0.7 km. We also show that even if there is an luminosity, sampling the light curves on timescales spanning from unmodeled nonthermal component modulated at the pulsation few hundred seconds to years. We use our measurements of frequency, good statistical fits could rule out significant biases. The dynamic ranges, duty cycles as a function of luminosity, and low count rate will make reliable upper limits on the radius luminosity distributions to highlight systematic differences that difficult, but the lower limit could rule out some equations of state help discriminate between different theoretical models proposed to that are currently being discussed. This analysis would require a explain the differences between the wind accretion processes in good estimate of the non-source background, so Chandra SFXTs and classical SGXBs. Our follow-ups of the SFXT outbursts observations of the vicinity of PSR J1614-2230 would be important. provide a steady advancement in the comprehension of the mechanisms triggering the high X-ray level emission of these sources. In particular, the recent observations of the outburst of Author(s): M. Coleman Miller1 the SFXT prototype IGR J17544-2619 on 2014 October 10, when Institution(s): 1. Univ. of Maryland the source reached a peak luminosity of 3x1038 erg s -1 , challenged, for the first time, the maximum theoretical luminosity achievable 120.18 – The Quiescent Neutron Star and Hierarchical by a wind-fed neutron star high mass X-ray binary. We propose Triple, 4U2129+47 that this giant outburst was due to the formation of a transient 4U 2129+47 is a quiescent, eclipsing neutron star that 35 years ago accretion disc around the compact object. showed typical "Accretion Disk Corona" (ADC) behavior akin to the Author(s): Patrizia Romano2, Jamie Kennea5 , Scott Douglas prototype of the class, X1822-371. Now faded, 4U 2129+47 43 5 7 provides tests of neutron star quiescent emission. It has shown low Barthelmy , Enrico Bozzo , David N. Burrows , Lorenzo Ducci , Paolo Esposito16 , Phil Evans , Neil Gehrels 4 , Hans A. Krimm 4 , temperature thermal emission (the neutron star surface), a power 2 law tail (of unknown origin, although possibly due to a pulsar wind Stefano Vercellone interacting with an incoming accretion stream; Campana et al. Institution(s): 1. INAF-IASF Milano, 2. INAF-IASF Palermo, 3. 1998), and sinusoidally modulated absorption (the disk) as well as ISDC, 4. NASA's GSFC, 5. Penn State, 6. University of Leicester, 7. periodic X-ray eclipses. Subsequent XMM-Newton and Chandra University of Tuebingen observations, taken 2007 through Fall 2015, indicate that the hard tail and sinusoidal modulation disappeared, as if the accretion 120.21 – RXTE Observations of Positive Correlations stream and disk have vanished. With the intiial loss of the hard tail, between the Cyclotron Line Parameters and the soft X-ray flux also dropped, but since has remained steady, Luminosity in GX 304-1 showing no signs of further neutron star cooling in the subsequent The Rossi X-ray Timing Explorer observed four outbursts of the 8 years. We compare this behavior to recent NuSTAR observations accreting X-ray binary transient source GX 304-1 in 2010 and 2011. of the quiescent neutron star Cen X-4, where the hard tail seems to During the 2010-2011 observations, the HEXTE cluster A viewing persist over a wider range of quiescent flux, and correlate with the direction was fixed aligned with the PCA field of view and HEXTE soft X-ray. It also has been speculated that 4U 2129+47 is part of a cluster B was fixed viewing a background region 1.5 degrees off of hierarchical triple system, with the third body in a much longer the source direction. The cluster A background was successfully estimated from cluster B events, and this made possible the Rossi X-ray Timing Explorer (RXTE). We have developed a burst measurement of the ~55 keV cyclotron line and an accurate model employing the Schwarzschild + Doppler approximation for measurement of the continuum. The cyclotron line energy spans surface emission coupled with realistic flame spreading geometries 50 to 60 keV throughout each outburst, implying magnetic fields and burst cooling to compute light curves and oscillation ranging from 4-5 teraGauss as the scattering region reacts to the amplitudes for both the rising and cooling phases of X-ray bursts. varying mass accretion rate. We present results of a detailed 3-100 We use this model to explore the capabilities for the Neutron star keV spectral analysis of 69 separate observations, and report a Interior Composition ExploreR (NICER) to detect and study burst greater than 7 sigma measurement of a positive correlation oscillations, particularly in the energy band below 3 keV. NICER is between cyclotron line parameters (energy, width, and depth) and an International Space Station attached payload (X-ray telescope) luminosity, as well as other spectral parameters' correlations with with capabilities optimized for fast timing of neutron stars in the luminosity. The three cyclotron line parameters’ correlations with 0.2–10 keV band. It has large collecting area (twice that of the luminosity show a flattening of the relationships with increasing XMM-Newton EPIC-pn camera), CCD-quality spectral resolution, luminosity, and have been fitted by quasi-spherical accretion and and high-precision time tagging referenced to UTC through an disk accretion models. The width and depth correlation exponents onboard GPS receiver. NICER will begin its 18-month prime follow directly from the energy correlation exponent with only the mission around the end of 2016. We will present results of assumption that the accretion column is in the subcritical simulated X-ray bursts with NICER that explore its burst (Coulomb-braking) regime and the energy changes in proportion oscillation detection capabilities and prospects for inferring to the characteristic stopping length of protons. Correlations of all neutron star properties from phase-resolved spectra. spectral parameters with primary 2-10 keV power law flux reveal the mass accretion rate to be the primary driver of the spectral shape. A large enhancement in the line of sight column density Author(s): Tod E. Strohmayer1, Simin Mahmoodifar1 lasting about three days is seen just before periastron in one Institution(s): 1. NASA's GSFC outburst and a smaller enhancement of similar duration at the same orbital phase is seen in a second outburst, suggesting the 120.24 – The NuSTAR X-ray Spectrum of Hercules X-1: presence of a dense structure in the stellar wind. A Radiation-Dominated Radiative Shock We report on new spectral modeling of an observation of the accreting X-ray pulsar Her X-1 by the Nuclear Spectroscopic 2 3 Author(s): Richard E. Rothschild , Matthias Kühnel , Paul Telescope Array (NuSTAR). We utilize a radiation-dominated Britton Hemphill22 , Alex Markowitz , Katja Pottschmidt 4 , Joern 355 radiative shock model that is an implementation of the analytic Wilms , Rüdiger Staubert , Dmitry Klochkov , Konstantin work of Becker & Wolff (2007) on Comptonized accretion flows 11 Postnov , Mikhail Goronostaev onto magnetic neutron stars within the XSPEC analysis Institution(s): 1. Moscow State University, 2. UC, San Diego, 3. environment. We obtain a good fit to the Her X-1 spin-phase University of Erlangen, 4. University of Maryland, Baltimore averaged 4 to 78 keV X-ray spectrum observed by NuSTAR during County, 5. University of Tuebingen a main-on phase of the Her X-1 35-day accretion disk precession period. This model allows us to estimate the accretion rate, the 120.22 – Modeling Neutron Star and Galactic Black Comptonizing temperature of the radiating plasma, the radius of Hole Emission: The Impact of Proper Extinction the magnetic polar cap, and the average scattering opacity Calculations parameters in the accretion column. This is in contrast to previous Interstellar extinction includes both absorption and scattering of spectral models that characterized the shape of the X-ray spectrum photons from interstellar gas and dust grains, and it has the effect but could not determine the physical parameters of the accretion of altering a source's spectrum and its total observed intensity. flow. We describe the details of our spectral fitting model and we However, while multiple absorption models exist, there are no discuss the interpretation of the resulting accretion flow physical useful scattering models in standard X-ray spectrum fitting tools, parameters. such as XSPEC. Nonetheless, X-ray halos, created by scattering from dust grains, are detected around even moderately absorbed This research is supported by the NASA Astrophysics Data Analysis sources and the impact on an observed source spectrum can be Program. significant, if modest, compared to direct absorption. By convolving the scattering cross section with dust models, we have created a Author(s): Michael Thomas Wolff4, Peter A. Becker3 , Amy spectral model as a function of energy, type of dust, and extraction Gottlieb61 , Felix Fuerst , Paul Britton Hemphill 5 , Diana Marcu- region that can be used with models of direct absorption. This will Cheatham66 , Katja Pottschmidt , Fritz-Walter Schwarm 2 , Joern ensure the extinction model is consistent and enable direct Wilms24 , Kent Wood connections to be made between a source's X-ray spectral fits and Institution(s): 1. California Institute of Technology, 2. Dr. its UV/optical extinction. I will present the model and show its Karl-Remeis-Sternwarte and ECAP, 3. George Mason University, impact on a range of Galactic sources including neutron stars and 4. NRL, 5. University of California, San Diego, 6. University of black holes. Maryland Baltimore County

Author(s): Randall K. Smith3, Lynne A. Valencic1 , Lia 120.25 – Decoding the heartbeat of the microquasar Corrales2 GRS 1915+105: Disk wind Connection Institution(s): 1. Johns Hopkins University, 2. MIT, 3. GRS 1915+105 is a microquasar that shows extreme variability in Smithsonian Astrophysical Observatory X-ray, IR and radio bands. It shows disk emission, relativistic jets and strong winds during its different states. We observed this 120.23 – X-ray Bursts and Oscillations: Prospects with source recently with NuSTAR and Chandra during the heartbeat NICER state, characterized a 50 seconds strong oscillations. The X-ray bursts (Type I) are produced by thermonuclear flashes in the oscillations are likely due to thermal/viscous instability in the inner accreted surface layers of some neutron stars in Low Mass X-ray disk when it deviates significantly from the standard Shakura & Binaries (LMXBs). High frequency oscillations are observed during Sunyaev disk. Combining the high sensitivty of Nustar and the some of these bursts. These "burst oscillations" result from high resolution of Chandra, we use phase spectroscopy to study the rotational modulation of an inhomogeneous temperature details of these oscillation, revealing changes in the inner accretion distribution on the neutron star surface induced by ignition and disk as well as the launching of powerful winds during the subsequent spreading of the thermonuclear flash. They provide a oscillations. I will discuss the implications of these results on means to measure the spin rates of accreting neutron stars and accretion physics, the thermal instability and the launching since the burst emission arises from the neutron star surface, a mechanism of the wind. unique probe of neutron star structure. To date, virtually all observations of such oscillations have been made with NASA's Author(s): Abderahmen Zoghbi2, Jon M. Miller2 , Fiona spectrum is expected to increase with increasing energy above 8 Harrison1 keV, while the observed lags in 4U 1608-52 show the opposite Institution(s): 1. Caltech, 2. University of Michigan behavior. This demonstrates that the lags in the lower kHz QPO of 4U 1608-52 are not solely due to reverberation. We do note, 120.26 – A deep census of the X-ray binary however, that the models appear to be more consistent with the populations in the SMC much flatter lag energy spectrum observed in the upper kHz QPO The analysis of the deep Chandra survey of the Small Magellanic of several neutron star low-mass X-ray binaries, suggesting that Cloud (SMC) (a Chandra X-ray Visionary Program) yielded a lower and upper kHz QPOs may have different origins. wealth of discrete X-ray sources down to a limiting luminosity of a Author(s): Edward Cackett1 few times 1032 erg/s. The survey is designed to sample stellar Institution(s): 1. Wayne State University populations of ages between ~10 up to ~100Myr, in order to study the evolution of the X-ray binary populations as a function of age. Based on the comparison of the detected X-ray sources with 120.29 – Comparison of a third Anomalous Low State photometric catalogs of the SMC, we identify over 100 High Mass with a Normal Low State in LMC X-3 with MAXI, Swift, X-ray binaries (HMXBs) associated with the SMC, 21 of which and XMM-Newton exhibit pulsations. We measure the formation rate of HMXBs as a LMC X-3 is a bright, unusual black hole X-ray binary with function of the age of their parent stellar populations, and we find high-amplitude, non-periodic long-term variability on the order of that it shows a clear peak at ages of ~30-40Myr. In addition we hundreds of days, much longer than its 1.7-day orbital period. This measure the X-ray luminosity function of HMXBs which shows a long-term variability is believed to be caused by a mass accretion clear break at a luminosity of ~5×1034 erg/s, indicative of the onset rate change because of an observed lag of the X-rays behind the of the propeller effect. We discuss these results in the context of UV. We have also found LMC X-3 to undergo anomalous low X-ray binary populations in environments of different ages and states (ALSs) in which its flux drops dramatically by a factor of metallicities. about 1000 and stays low for at least 80 days or more. This was last observed in late 2011 into early 2012. LMC X-3 has a rich dataset Author(s): Andreas Zezas4, Vallia Antoniou11 , JaeSub Hong , including observations from JAXA’s MAXI, NASA’s RXTE and Nick Wright213 , Jeremy J. Drake , Frank Haberl , & The SMC XVP Swift, and as well as ESA’s XMM-Newton. MAXI has continuously Collaboration1 monitored the system since 2009 and has excellent coverage of the Institution(s): 1. Harvard-Smithsonian CfA, 2. Keele University, most recent ALS. Swift XRT and UVOT observations have good 3. MPE, 4. SAO coverage of LMC X-3’s egress into the ALS as well as complete coverage of an additional normal low state. Using these 120.27 – Two methods for studying the X-ray observations we study the behavior of the system as it enters and variability exits these states in order to quantify the differences in LMC X-3’s The X-ray aperiodic variability and quasi-periodic oscillation (QPO) characteristics during an ALS versus normal low state. The ALS has are the important tools to study the structure of the accretion flow a minimum flux upper limit of ~0.06 mCrab as measured by Swift, of X-ray binaries. However, the origin of the complex X-ray while the minimum flux of the normal low state is ~8 mCrab --- variability from X-ray binaries remains yet unsolved. We proposed more than 130 times brighter. There are also 4 XMM-Newton two methods for studying the X-ray variability. One is observations that track LMC X-3’s entrance into the ALS, with the amplitude-ratio spectrum analysis method. The other is mapping final observation occurring squarely within the ALS. These data analysis method. Based on the consideration that the aperiodic reveal a greater than 7500x drop in flux over that time frame. We variability originates from all spectral components whereas the model these spectra to measure LMC X-3’s spectral evolution into QPO originates from one spectral component, we divided the the ALS, and also report what is currently the best measurement root-mean-square (rms) amplitude spectrum of the power density we have of the source flux while in an ALS (~0.001 mCrab, which spectrum (PDS) broadband noise component by the amplitude corresponds to less than 2x10-5 Ledd ). spectrum of an accompanying QPO, and first identified a Author(s): Trevor Torpin1, Patricia T. Boyd33 , Alan P. Smale , high-frequency (> 10 Hz) aperiodic variability from the accretion 2 disk (Yan et al. 2013). We now present the evolution of the Lynne A. Valencic amplitude-ratio spectrum with the cycle phase of the heartbeat Institution(s): 1. Catholic University of America, 2. Johns state of the microquasar GRS 1915+105. We produced the energy- Hopkins University, 3. NASA's Goddard Space Flight Center frequency-power map to investigate the origin of the X-ray variability, and show that most aperiodic X-ray variability is 120.30 – The Unusual Long Term Variability of LMXB produced in the corona, and the low-frequency aperiodic variability 4U 1705-440---Fingerprints of Chaotic Evolution? from the corona is significant in the hard phase of the cycle phase The bursting Atoll source 4U 1705-44, exhibits high amplitude, of the heartbeat state of GRS 1915+105 while the low-frequency long-term aperiodic variability on characteristic timescales of aperiodic variability from the disk and the corona are both several hundred days. The brightness of the system makes it significant in the soft phase. continuously observable by a variety of all-sky monitors. We combine data from te All-Sky Monitor (ASM) aboard the Rossi Author(s): Shu-Ping Yan3, Li Ji32 , Mariano M\'endez , Na X-ray Timing Explorer (RXTE) and MAXI, the Japanese X-ray Wang43 , Siming Liu , Xiang-Dong Li 1 All-Sky Monitor aboard the International Space Station, resulting Institution(s): 1. Department of Astronomy, Nanjing University, in a continuous, uninterrupted, evenly spaced time series 2. Kapteyn Astronomical Institute, University of Groningen, 3. containing over fifty cycles at the timescale of interest. We Purple Mountain Observatory, CAS, 4. Xinjiang Astronomical construct a two-dimensional phase space from the flux versus its Observatory, CAS first derivative, and find a strong resemblence to the canonical double-welled nonlinear Duffing osciallator. We uncover several 120.28 – Are the kHz QPO lags in neutron star 4U low-order unstable periodic orbits embedded in the light curve of 1608-52 due to reverberation? 4U 1705-44, which imply that the "period-1" orbit lasts ~120 days. X-ray reverberation lags have recently been discovered in both We find clear signatures of period-1, period-2 and period-3 orbits active galactic nuclei (AGN) and black hole X-ray binaries. A recent and extract these to calculate their topological behavior in phase study of the neutron star low-mass X-ray binary 4U 1608-52 has space. The topoligical relations suggest that the equations also shown significant lags, whose properties hint at a describing the long term evolution of 4U 1705-44 are similar to reverberation origin. Here, we adapt general relativistic ray tracing those of the Duffing oscillator. This puts limits on the allowable impulse response functions used to model X-ray reverberation in models describing the longterm variability of 4U 1705-44 and, by AGN for neutron star low-mass X-ray binaries, and calculate the extention, to the allowable models describing other systems which expected lags as a function of energy over the range of observed show non-periodic superorbital variability. kHz QPO frequencies in 4U 1608-52. We find that the lag energy Author(s): Patricia T. Boyd2, Rebecca Phillipson1 , Alan P. describe the X-ray binary’s variability. Smale2 Institution(s): 1. Drexel University, 2. NASA's GSFC Author(s): Rebecca Phillipson1, Patricia T. Boyd2 , Alan P. Smale2 120.31 – The Masses of Black Holes with Wolf-Rayet Institution(s): 1. Drexel University, 2. NASA Goddard Space Companions Flight Center Black Holes with Wolf-Rayet companions represent a channel for forming the most massive stellar BHs. The recent, stunning LIGO 120.33 – Comparing the spatial distributions of detection of the gravitational wave signature from a merging stellar HMXBs and star-forming regions in the Small BH binary points to the importance of understanding the Magellanic Cloud progenitor systems formation and evolution. The BH+WR binary Initial results are presented comparing the spatial distribution of IC 10 X-1 holds important clues to the puzzle, by helping establish high-mass X-ray binaries (HMXBs) and massive stellar nurseries the upper observed BH mass and pointing to an association (OB associations) in the Small Magellanic Cloud (SMC). The between maximum possible BH mass and low metallicity analysis involves constructing the two-point cross-correlation environments. However, securing dynamical mass determiniations function between pairs of 72 HMXBs and 234 OB associations with for WR+BH binaries appears to be complicated by interaction the latter being randomly reshuffled following a homogenous between the radiation field of the BH and the stellar wind. This distribution, a Gaussian distribution, and a distribution that causes a substantial change to our understanding of IC 10 X-1, and mimics the star-formation history of the SMC. We find a significant by extension to the mass distribution of BH binaries. A high (>5-sigma) correlation between the observed HMXB and OB precision ephemeris derived from a decade of Chandra/XMM catalogs compared with a random catalog in which the OB X-ray timing observations, when combined with the optical RV associations are distributed homogeneously across the SMC field. curve, reveals a surprizing simultenaity of mid X-ray eclipse and On average, within a kpc of a given HMXB, there are 4 OB the maximum blueshift velocity of He II emission lines. The optical associations from the observed catalog for every one from the emission lines appear to originate in a shielded sector of the WR randomized catalog. There is no significant difference when star's stellar wind which escapes total X-ray ionization by the comparing the HMXBs with the observed catalog versus the compact object. Unravelling this projection effect is necessary to random catalog in which the OB distribution traces the obtain the system's true mass function. Complementary Chandra, star-formation history. This suggests that HMXBs in the SMC have XMM and NuStar datasets offer new insights into the mass and had less time to migrate away from their birthplaces (or, spin of the BH, and the structure of the photo-ionized wind. We alternatively, that they have a lower average velocity) than HMXBs will discuss possible routes toward the mass function in BH+WR in the Milky Way. One explanation is that the HMXBs in our binaries via multi-wavelength observations, and the additional sample all host B-emission-line stars that have not yet left the main leverage provided by further constraining the orbital period sequence. derivative. Author(s): Arash Bodaghee3, Vallia Antoniou2 , Andreas Author(s): Silas Laycock31 , James F. Steiner , Thomas J. Zezas2311 , John Tomsick , Ryan Agnew , Eric Frechette , Brenton Maccarone234 , Dimitris M. Christodoulou , Breanna A. Binder , Jun Jackson11 , Zachary Jordan Yang33 , Rigel Cappallo Institution(s): 1. Georgia College, 2. Harvard CfA, 3. University Institution(s): 1. MIT Kavli Institute, 2. Texas Tech., 3. of California, Berkeley University of Massachusetts, 4. University of Washington

120.32 – Investigating the Long-term Variability of 200 – Solar Wind Charge Exchange: 4U1705-44; Evidence for an Underlying Nonlinear Double-Welled Oscillator Measurements and Models The bright low-mass X-ray binary 4U1705-44 exhibits long-term 200.02 – Models of Heliospheric solar wind charge semi-periodic variability with a timescale of several hundred days. exchange X-ray emission The All-Sky Monitor (ASM) aboard the Rossi X-ray Timing The first models of the solar wind charge exchange (SWCX) X-ray Explorer (RXTE) and the Japanese X-ray All-Sky Monitor (MAXI) production in the heliosphere were developed shortly after the aboard the International Space Station together have continuously discovery of SWCX emission at the end of 1990s. Since then, observed the source from December 1995 through the present. The continuous monitoring of the global solar wind evolution through combined ASM-MAXI data provides a continuous time series over the solar cycle has allowed better constraints on its interaction with fifty times the length of the timescale of interest. The phase space the interstellar neutrals. We have a fairly accurate description of embedding of the flux versus its first derivative shows a strong the interstellar neutral density distributions in interplanetary resemblance to a double-welled nonlinear oscillator. When space. However, the solar wind heavy ion fluxes, and especially comparing our time series against well-known nonlinear their short term variability and propagation through interplanetary oscillators, we find that 4U1705-44 exhibits behavior akin to the space, have remained relatively elusive due to the sparseness or Duffing oscillator. Topological analysis can help us identify lack of in situ data, especially towards high ecliptic latitudes. In this ‘fingerprints’ in the phase space of a system unique to its equations talk, I will present a summary the heliospheric SWCX modeling of motion. If such ‘fingerprints’ are the same between two systems, efforts, and an overview of the global solar cycle variability of then their equations of motion must be closely related. We heliospheric SWCX emission, while commenting on the difficulties therefore found a range of parameters for which the Duffing of modeling the real-time variability of the heliospheric X-ray oscillator closely follows the time evolution of 4U1705-44 and from signal. this range chose 6 different numerical Duffing time series. We can extract low-period, unstable periodic orbits from both the Author(s): Dimitra Koutroumpa1 4U1705-44 and numerical Duffing time series and compare their Institution(s): 1. LATMOS - CNRS - IPSL topological information in phase space, such as their relative rotation rates. We argue that the associated period-1 orbit in 200.03 – Solar Wind Charge Exchange X-ray Emission 4U1705-44 has a period between 130 and 170 days. The driving from Earth's Magnetosheath periods of our 6 numerical time series correspond to 140 to 175 days. Assigning a logical sequence name to each orbit, the relative The magnetospheric component of solar wind charge-exchange rotation rates can be compiled into a unique ‘intertwining’ matrix. (SWCX) emission is primarily due to interaction between the The numerical Duffing time series and the 4U1705-44 intertwining high-state ions in the solar wind and the hydrogen in the matrices are identical, which provides strong evidence that they outermost part of the Earth’s atmosphere. This emission was the share the same underlying template. The implications of this primary source of the ROSAT long-term enhancements (LTEs). equivalence suggests that we can look to the Duffing equation to Using the correlation between the LTEs and the solar wind flux as well as a dynamic models of the magnetosheath, we have derived Theory and Observations of Accretion the 1/4 keV broad-band charge-exchange cross-section, and can show that this method can not be directly applied to the 3/4 keV Column Physics band. I will discuss the uncertainties in this method and the 201.01 – Overview of the physics in the accretion prospects for improvement. column Author(s): Steve L Snowden2, K. D. Kuntz1 This talk discusses the current efforts to model the wide array of Institution(s): 1. JHU, 2. NASA/GSFC physical processes that are important when plasma accretes onto the surface of a highly magnetic neutron star. Broad non-thermal 200.04 – DXL: A sounding rocket mission measuring power law X-ray continua are observed that can be modeled by Solar Wind Charge eXchange properties Comptonization of bremsstrahlung, cyclotron, and black body contributions. Cyclotron resonance absorption lines are observed, Solar Wind interacts with the interstellar neutrals via charge cast against these broad continua, yielding measurements of the exchange mechanism to produce spatially and temporally varying magnetic field strengths. Observations show that in some sources x-rays making it difficult to separate from other diffuse sources. the cyclotron line energies can vary with observed luminosity. This The Diffuse X-rays from the Local Galaxy (DXL) mission measured observation has lead to significant debate regarding aspects of the the spatial signature of Solar Wind Charge eXchange (SWCX) cyclotron line formation process. Multiple groups are currently emission due to the helium focusing cone. The mission used 2 working on modeling the physical processes that affect the large area proportional counters and was able to separate the behavior of the plasmas, the formation of the X-ray continuum, SWCX contribution from Local Hot Bubble emission. The data and the formation of the cyclotron lines. New analysis tools are from the mission provide a robust estimate of the SWCX becoming available to help interpret observations of these systems. contribution to the ROSAT maps, measuring the compound SWCX In particular, observations by Suzaku and NuSTAR of the X-ray cross section with He in all ROSAT bands. The results showed that spectra of these binary systems are advancing our searches for the the total SWCX contribution in the ¼ keV band is, on average, cyclotron lines and our understanding of the physical processes ~27%. A new mission, DXL-2, was launched on December 4, 2015 that contribute to the X-ray continuum formation. with two new counters for a better understanding of the energy distribution of heliospheric SWCX photons, by using a multi-band Author(s): Michael Thomas Wolff1 approach. A dedicated scan to accurately measure the cone position Institution(s): 1. NRL and solve the IBEX controversy was also performed. The talk will discuss the DXL mission, the results from the first flight, and the 201.02 – Application of a physical continuum model to preliminary results from the latest flight. recent X-ray observations of accreting pulsars We present a uniform spectral analysis in the 0.5-50 keV energy Submitted for the DXL Collaboration range of a sample of accreting pulsars by applying an empirical broad-band continuum cut-off power-law model. We also apply the Author(s): Massimiliano Galeazzi1 newly implemented physical continuum model developed by Institution(s): 1. Univ. of Miami Becker and Wolff (2007, ApJ 654, 435) to a number of high-luminosity sources. The X-ray spectral formation process in 200.05 – The temperature and structure of the local this model consists of the Comptonization of bremsstrahlung, hot bubble from DXL mission cyclotron, and black body photons emitted by the hot, magnetically channeled, accreting plasma near the neutron star surface. This DXL (Diffuse X-rays from the Local Galaxy) is a sounding rocket model describes the spectral formation in high-luminosity mission designed to quantify and characterize the contribution of accreting pulsars, where the dominant deceleration mechanism is Solar Wind Charge eXchange (SWCX) to the diffuse X-ray via a radiation-dominated radiative shock. The resulting spectra background. Based on the results from the DXL mission, we depend on five physical parameters: the mass accretion rate, the estimated the SWCX contribution to the soft X-ray background radius of the accretion column, the electron temperature and from the Rosat All Sky Survey (RASS). After removing the SWCX electron scattering cross-sections inside the column, and the contamination, we were able to measure the temperature and magnetic field strength. The empirical model is fitted to Suzaku emission measure of the “cleaned” local hot bubble, and to build its data of a sample of high-mass X-ray binaries covering a broad 3-Dimensional structure. luminosity range (0.3-5 x 10 37 erg/s). The physical model is fitted to Suzaku data from luminous sources: LMC X-4, Cen X-3, GX 304-1. We compare the results of the two types of modeling and Submitted for the DXL Collaboration summarize how they can provide new insight into the process of Author(s): Wenhao Liu1 accretion onto magnetized neutron stars. Institution(s): 1. University of Miami Author(s): Diana Monica Marcu-Cheatham7, Katja Pottschmidt743 , Michael Thomas Wolff , Peter A. Becker , Kent S. 200.06 – New Missions and the Future of Solar Wind Wood42 , Joern Wilms , Paul Britton Hemphill 5 , Amy Gottlieb 6 , Charge Exchange Studies Felix Fuerst122 , Fritz-Walter Schwarm , Ralf Ballhausen Several newly approved missions in astrophysics and heliophysics Institution(s): 1. Caltech, 2. FAU-Erlangen Nuremberg, 3. will study solar wind charge-exchange (SWCX) directly as either George Mason University, 4. NRL, 5. UCSD, 6. UFL, 7. UMBC primary or secondary science goals. Of these, SMILE and CuPID will study the magnetosheath by means of the SWCX emission and 201.03 – Physics of Cyclotron Resonance Scattering will provide a direct measure of the magnetospheric emission from Features in both the 1/4 keV and 3/4 keV bands. HaloSAT observations will Cyclotron resonant scattering features (short: cyclotron lines) are be designed to minimize the magnetospheric component for its sensitive tracers of the physics of the accretion columns and observations of the Galactic Halo, but will make at least some mounds of X-ray pulsars. They form by interaction of X-ray dedicated observations of heliospheric SWCX. I will outline the photons with magnetically quantized electrons in the accreted simulation needs and observational strategies required to study plasma close to the neutron star. Such lines have been observed as SWCX for astrophysical purposes. absorption-like features for about 20 X-ray pulsars. Their energies Author(s): K. D. Kuntz1 provide a direct measure of the magnetic field strength in the Institution(s): 1. Johns Hopkins Univ. line-forming region. By detailed modelling of the lines and of their parameter dependencies we can further decipher the physical conditions in the accretion column. For instance the fact that the complex scattering cross sections have a strong angle-dependence 201 – TeraGauss, Gigatons, and MegaKelvin: relates the phase-resolved cyclotron line shapes to parameters that constrain the systems’ still poorly understood geometry. Modelling reconfiguration of the structure of the accretion mound not the physics of cyclotron lines to a degree that allows for detailed reflected in the other spectral parameters. I will discuss the analysis and solid comparison to data therefore provides a unique access and some implications of this result, especially in the context of also to a better understanding of the overall picture of magnetically work by Staubert et al. (2015, A&A 572, 119), which unveiled a accreting neutron star systems. secular trend in the CRSF energy of the prototypical CRSF source, Hercules X-1. Author(s): Gabriele Sschoenherr5, Fritz-Walter Schwarm1 , Sebastian Falkner11 , Thomas Dauser , Katja Pottschmidt 6 , Peter Author(s): Paul Britton Hemphill2, Richard E. Rothschild2 , Kretschmar234 , Dmitry Klochkov , Carlo Ferrigno , Paul Britton Felix Fuerst176 , Victoria Grinberg , Dmitry Klochkov , Peter Hemphill71 , Joern Wilms Kretschmar536 , Katja Pottschmidt , Rüdiger Staubert , Joern Institution(s): 1. ECAP / FAU Erlangen-Nuremberg, 2. ESA, 3. Wilms4 Institut for Astronomy and Astrophysics, University of Tuebingen, Institution(s): 1. Cahill Center for Astronomy and Astrophysics, 4. ISDC, 5. Leibniz-Institute for Astrophysics Potsdam (AIP), 6. California Institute of Technology, 2. Center for Astrophysics and NASA-GSFC, 7. University of California, San Diego Space Sciences, University of California, San Diego, 3. Center for Space Science and Technology, University of Maryland Baltimore 201.04 – Spectrum-luminosity dependence of County, 4. Dr. Karl Remeis-Sternwarte & Erlangen Center for radiation from the polar emitting regions in accreting Astroparticle Physics, 5. European Space Astronomy Center magnetized neutron stars (ESA/ESAC), 6. Institut für Astronomie und Astrophysik, The recent progress in observational techniques allowed one to Universität Tübingen, 7. Kavli Institute for Astrophysics, probe the evolution of the X-ray spectrum in accreting pulsars Massachusetts Institute of Technology (especially, of the cyclotron absorption line - the key spectral feature of accreting magnetized neutron stars) in great detail on 201.07 – Pulsar observations with NuSTAR various timescales, from pulse-to-pulse variability to secular The Nuclear Spectroscopic Telescope Array (NuSTAR) is the first trends. Particularly interesting are the discovered spectrum- focusing hard X-ray telescope in orbit and ideally suited to study luminosity correlations which are being used to infer the structure cyclotron lines (CRSFs), due to its good spectral resolution above and physical characteristics of the pulsar's polar emitting region. I 10keV and very high signal-to-noise ratio. I will review the results will present the latest developments in the modeling of the emitting from the first 3 years of NuSTAR observations and describe how structure (accretion column/mound/spot) aimed at explaining the NuSTAR contributes to the discovery and detailed study of CRSFs. observed spectrum-luminosity dependences. NuSTAR has discovered a CRSF in KS 1947+319, 4U 1538-22, and 2S 1553-542, increasing the small sample of about 25 known CRSF Author(s): Dmitry Klochkov1 sources. NuSTAR was also responsible for discovering a luminosity Institution(s): 1. Institut for Astronomy and Astrophysics, dependence of the CRSF energy in Vela X-1 at very low University of Tuebingen luminosities, as well as measuring an asymmetric line profile for the first time in Cep X-4. I will conclude with a brief outlook into 201.05 – Long-term change in the cyclotron line future NuSTAR observations and plans. energy in Her X-1 Author(s): Felix Fuerst1, MAGNET collaboration1 We investigate the long-term evolution in the centroid energy of Institution(s): 1. Caltech the Cyclotron Resonance Scattering Feature (CRSF) in the spectrum of the binary X-ray pulsar Her X-1. After the discovery in 1976 by the MPE/AIT balloon telescope HEXE, the line feature was 201.08 – Self consistent modeling of accretion confirmed by several other instruments, establishing the centroid columns in accretion powered pulsars energy at around 35 keV, thereby providing the first direct measure We combine three physical models to self-consistently derive the of the B-filed strength of a neutron star at a few 10^12 Gauss. observed flux and pulse profiles of neutron stars' accretion Between 1991 and 1993 an upward jump by ~7 keV occurred, first columns. From the thermal and bulk Comptonization model by noted by BATSE and soon confirmed by RXTE and Beppo/SAX. Becker & Wolff (2006) we obtain seed photon continua produced Since then a systematic effort to monitor the cyclotron line energy in the dense inner regions of the accretion column. In a thin outer E_cyc with all available instruments has led to two further layer these seed continua are imprinted with cyclotron resonant discoveries: 1) E_cyc correlates positively with the X-ray scattering features calculated using Monte Carlo simulations. The luminosity (this feature is now found in four more binary X-ray observed phase and energy dependent flux corresponding to these pulsars). 2) Over the last 20 years the (flux normalized) E_cyc in emission profiles is then calculated, taking relativistic light bending Her X-1 has decayed by ~5 keV, down to 36.5 keV in August 2015. into account. We present simulated pulse profiles and the predicted Her X-1 is the first and so far the only source showing such a dependency of the observable X-ray spectrum as a function of variation. We will discuss possible physical scenarios relevant for pulse phase. accretion mounds/columns on highly magnetized neutron stars. Author(s): Sebastian Falkner3, Fritz-Walter Schwarm3 , Author(s): Rüdiger Staubert1 Michael Thomas Wolff213 , Peter A. Becker , Joern Wilms Institution(s): 1. University of Tübingen Institution(s): 1. George Mason University, 2. Naval Research Laboratory, 3. University of Erlangen-Nuremberg 201.06 – Evidence for an Evolving Cyclotron Line Energy in 4U 1538-522 In this talk, I present results from a comprehensive analysis of the 202 – The Structure of the Inner Accretion existing RXTE, INTEGRAL, and Suzaku data for the high-mass Flow of Stellar-Mass and Supermassive X-ray binary 4U 1538-522. This persistent X-ray pulsar has a clearly-detected cyclotron resonance scattering feature (CRSF), Black Holes which appears to have increased in energy over the past decade, from approximately 20-21 keV as measured by RXTE in 1996-2004 202.01 – Observations of Relativistically Broadened to ~22-23 keV as found in the 2012 Suzaku observation. This Iron K-Alpha Lines from AGNs spectral feature is the only direct measurement of the neutron Relativistic X-ray reflection is commonly seen in many unobscured star's magnetic field strength, and its behavior can be used to track AGN. The iron K-alpha line is usually its most prominent feature. the conditions in the accretion mound near the neutron star Observations of broad iron lines from ASCA to NUSTAR will be surface. Our analysis finds that the increased CRSF energy is reviewed and their use in measuring the location and shape of the especially prominent in spectra from the peak of the main pulse, corona which suggests that the physical origin of this shift in energy may outlined. They also provide a measure of the spin of the black hole, be restricted to a single magnetic pole, possibly indicating some which is often found to be high. Selection effects involved here will be discussed. super-Eddington accretion disks. The properties of such flows will be described in detail and compared with observed characteristics Author(s): Andrew C Fabian1 of ULXs and X-ray binaries. I will also address the question of Institution(s): 1. University of Cambridge thermal stability of radiatively efficient accretion disks.

202.02 – Observations of Relativistically Broadened Author(s): Aleksander Sadowski1 Iron Kalpha Lines From Stellar Mass Black Holes Institution(s): 1. MIT The measurement of Doppler broadened and gravitationally redshifted iron emission lines from accreting black holes has been 202.06 – X-ray Spectra from GRMHD Simulations of used to measure the inner radius of the optically thick disk (Rin). Accreting Black Holes At high mass accretion rates, when the disk is at or close to the We present the results of a global radiation transport code coupled Innermost Stable Circular Orbit (ISCO), a determination of Rin to general relativistic magnetohydrodynamic (GRMHD) provides a constraint on the spin of the black hole. Measuring Rin simulations of accreting black holes. For the first time, we are able can also provide information about whether the disk is truncated or to explain from first principles in a self-consistent way all the not, and this is especially important for understanding the components seen in the X-ray spectra of stellar-mass black holes, relationship between the disk and the steady jet in the hard state. including a thermal peak and all the features associated with strong Over the past few years, the Nuclear Spectroscopic Telescope Array hard X-ray emission: a power law extending to high energies, a (NuSTAR) has provided improved measurements due to its Compton reflection hump, and a broad iron line. Varying only the combination of bandpass (3-79 keV), good energy resolution, and mass accretion rate, we are able to reproduce a wide range of X-ray high throughput. In this presentation, we discuss NuSTAR results states seen in most galactic black hole sources. The temperature in for a number of stellar mass black holes (e.g., Cyg X-1, GX 339-4, the corona is Te ~ 10 keV in a boundary layer near the disk and and GRS 1739-278). While these observations have been rises smoothly to Te >~ 100 keV in low-density regions far above successful in obtaining measurements of Rin, the improved spectra the disk. We self-consistently solve for the ionization state of gas in have also provided extra information about the source geometry each vertical column of the disk, in turn giving iron fluorescent and the inner disk inclination, which we will discuss. emissivity profile.

Author(s): John Tomsick1 Author(s): Jeremy Schnittman2, Scott Noble3 , Julian H. Institution(s): 1. UC Berkeley/SSL Krolik11 , Brooks Kinch Institution(s): 1. Johns Hopkins University, 2. NASA/GSFC, 3. 202.03 – Recent X-ray Reverberation Mapping University of Tulsa Results In recent years, X-ray reverberation has opened a new way to investigate the inner accretion flow around black holes. 203 – Missing Baryons and the Hot Halo of XMM-Newton and NuSTAR observations of the high-frequency variability have shown that the soft excess, broad iron K line and the Milky Way Compton hump lag behind the continuum emission, suggesting 203.01 – Missing metals and baryons in galaxies: light travel distances of a few gravitational radii. Beyond simply Clues from our Milky Way detecting reverberation, we are beginning to use reverberation to It is well-known that most galaxies are missing most of their map out the geometry of the inner accretion flow, testing the baryonic mass. Perhaps more surprisingly, they also seem to be compactness of the X-ray emitting source, the structure of the disc missing most of their metals. Our Milky Way galaxy, like other and the origin of the variability. In this talk, I will give an overview nearby galaxies, is missing most of its baryons. Cosmological of the observational results discovered thus far, and will discuss simulations of galaxy formation suggest that the missing baryonic future prospects for reverberation with upcoming observations and mass should reside in the circum-galactic medium (CGM), in a telescopes. warm-hot gas phase at temperatures between one million and 10 Author(s): Erin Kara1 million K. Although theoretical models predict the existence of the Institution(s): 1. University of Maryland warm-hot gas in the CGM, detecting and characterizing the diffuse CGM has been difficult. At the expected temperatures the baryons are in the form of highly ionized plasma, observable in soft X-rays. 202.04 – Modeling the Compton Hump Reverberation A combination of absorption and emission studies at soft X-ray Observed in Active Galactic Nuclei energies is required to fully characterize this warm-hot CGM. In recent years, observations of the Iron K alpha reverberation in Recently, combining the Chandra observations of OVII and OVIII supermassive black holes have provided a new way to probe the absorption lines and XMM-Newton and Suzaku measurements of inner accretion flow. Furthermore, a time lag between the direct the Galactic halo emission measure, we found that there is a huge coronal emission and the reprocessed emission forming the reservoir of ionized gas around the Milky Way, with the mass of Compton Hump in AGN has been observed. In order to model this over 2 billion solar masses and the radius of over 100 kpc. Compton Hump reverberation we performed general relativistic ray tracing studies of the accretion disk surrounding supermassive I will present Chandra, XMM-Newton and Suzaku observations black holes, taking into account both the radial and angular probing our Milky Way halo in absorption and emission. Our dependence of the ionization parameter. We are able to model results show that the Milky Way halo contains a huge reservoir of emission not only from a lamp-post corona but also implementing warm-hot gas that may account for a large fraction of missing 3D corona geometries. Using these results we are able to model the baryons and metals. I'll review current status of this field, discuss observed data to gain additional insight into the geometry of the implications of our results to models of galaxy formation and corona and the structure of the inner accretion disk. evolution and outline paths for future progress.

Author(s): Janie Hoormann1, Banafsheh Beheshtipour1 , Author(s): Anjali Gupta1 Henric Krawczynski1 Institution(s): 1. Columbus State Institution(s): 1. Washington University in St. Louis 203.02 – X-ray absorption/emission line spectroscopy 202.05 – Global simulations of sub- and super- of the Galactic hot gaseous halo Eddington black hole accretion disks in general There is an ongoing debate as to whether or not the Milky Way is relativity surrounded by a large-scale, massive corona. Vastly different In this talk I will review the recent progress in simulating optically conclusions as to its extent and mass have been drawn from thick black hole accretion flows. I will briefly describe the existing studies based on X-ray absorption and/or emission line computational methods and present simulations of both sub- and spectroscopy. I will discuss my assessment of this issue, focusing on various uncertainties and potential problems in the present Author(s): Philip Kaaret1 data, analyses, results, and interpretations. Institution(s): 1. Univ. of Iowa In particular, I will examine how different assumptions about the temperature distribution of the corona affect the inference of its physical scale. I will also discuss the external perspectives of 205 – Plenary Talk: Observation of galactic coronae obtained form observing nearby highly-inclined disk galaxies. Gravitational Waves in Advanced LIGO,

Author(s): Daniel Wang1 Laura Cadonati (Georgia Tech) Institution(s): 1. University of Massachusetts 205.01 – Observation of Gravitational Waves in Advanced LIGO 203.03 – The Crossroads between the Galactic Disk One hundred years after Einstein's formulation of General and Interstellar Space, Ablaze in 3/4 keV Light Relativity, LIGO has observed gravitational waves from a binary The halo is the crossroads between the Galactic disk and black hole merger. In this talk I will present this groundbreaking intergalactic space. This region is inhabited by hot gas that has discovery, which took place during the first observing run of risen from the disk, gas heated in situ, and hot material that has Advanced LIGO, and its implications for a new gravitational wave fallen in from intergalactic space. Owing to high spectral resolution astronomy. observations made by by XMM-Newton, Suzaku, and Chandra of the hot plasma's 3/4 keV emission and absorption, increasingly Author(s): Laura Cadonati1 sophisticated and CPU intensive computer modeling, and an Institution(s): 1. Georgia Tech awareness that charge exchange can contaminate 3/4 keV observations, we are now better able to understand the hot halo gas than ever before. 206 – Early Results from the Astro-H Spectral analyses indicate that the 3/4 keV emission comes from T ~ 2.2 million Kelvin gas. Although observations suggest that the Mission gas may be convectively unstable and the spectra's temperature is 206.01 – The ASTRO-H X-ray Observatory similar to that predicted by recent sophisticated models of the galactic fountain, the observed emission measure is significantly ASTRO-H, the new Japanese X-ray Astronomy Satellite following brighter than that predicted by fountain models. This brightness Suzaku, is an international X-ray mission, planed for launch in disparity presents us with another type of crossroads: should we Feb, 2016. ASTRO-H is a combination of high energy-resolution continue down the road of adding physics to already sophisticated soft X-ray spectroscopy (0.3 - 10 keV) provided by thin-foil X-ray modeling or should we seek out other sources? In this optics and a micro-calorimeter array, and wide band X-ray presentation, I will discuss the galactic fountain crossroads, note spectroscopy (3 - 80 keV) provided by focusing hard X-ray mirrors the latitudinal and longitudinal distribution of the hot halo gas, and hard X-ray imaging detectors. Imaging spectroscopy of provide an update on charge exchange, and explain how shadowing extended sources by the micro-calorimeter with spectral resolution observations have helped to fine tune our understanding of the hot of <7 eV can reveal line broadening and Doppler shifts due to gas. turbulent or bulk velocities. The mission will also carry an X-ray CCD camera as a focal plane detector for a soft X-ray telescope and Author(s): Robin L. Shelton1 a non-focusing soft gamma-ray detector based on a narrow-FOV Institution(s): 1. Univ. of Georgia semiconductor Compton Camera. With these instruments, ASTRO-H covers very wide energy range from 0.3 keV to 600 keV. 203.04 – A Rotation Signature in the Hot Halo of the The simultaneous broad band pass, coupled with high spectral Milky Way resolution by the micro-calorimeter will enable a wide variety of important science themes to be pursued. The hot halo of the Milky Way is massive and dynamically The ASTRO-H mission objectives are to study the evolution of important to the evolution of the Galaxy over cosmic time, so it is yet-unknown obscured super massive Black Holes in Active important to constrain its basic thermal, chemical, and structural Galactic Nuclei; trace the growth history of the largest structures in properties. The kinematic structure remains unknown, so we the Universe; provide insights into the behavior of material in measured the centroids of local OVII(r) absorbers seen towards extreme gravitational fields; trace particle acceleration structures in background quasars in XMM-Newton Reflection Grating clusters of galaxies and SNRs; and investigate the detailed physics Spectrometer data and compared them to simple models for bulk of jets. halo motion. The data rule out a stationary halo and suggest a ASTRO-H will be launched into a circular orbit with altitude of scenario in which the halo gas rotates at about 150 km/s in the about 575 km, and inclination of 31 degrees. prograde direction, at least within 50 kpc of the Sun. We also ASTRO-H is in many ways similar to Suzaku in terms of orbit, measured an inflow/outflow velocity consistent with zero. pointing, and tracking capabilities. After we launch the satellite, the Author(s): Edmund J. Hodges-Kluck1, Joel N. Bregman1 , current plan is to use the first three months for check-out and start Matthew J. Miller1 the PV phase with observations proprietary to the ASTRO-H team. Institution(s): 1. University of Michigan Guest observing time will start from about 10 months after the launch. About 75 % of the satellite time will be devoted to GO observations after the PV phase is completed. 203.05 – HaloSat – A CubeSat to Study the Hot In this presentation, we will describe the mission, scientific goal Galactic Halo and report the initial performance on the orbit. Observations of the nearby universe fail to locate about half of the normal matter (baryons) observed in the early universe. The Author(s): Tadayuki Takahashi1 missing baryons may be in hot galactic halos. HaloSat is a CubeSat Institution(s): 1. ISAS/JAXA designed to map oxygen line emission (O VII and O VIII) around the Milky Way in order to constrain the mass and spatial 206.02 – Progress report on the Astro-H Soft X-Ray distribution of hot gas in the halo. HaloSat has a grasp competitive Spectrometer with current X-ray observatories. Its observing program will be We describe the initial in-orbit operations and performance of the optimized to minimize contributions from solar wind charge Astro-H Soft X-Ray Spectrometer (SXS). Astro-H, JAXA's sixth exchange (SWCX) emission that limit the accuracy of current X-ray observatory, is scheduled for launch on February 12, 2016, measurements. We will describe the HaloSat mission concept, from the Tanegashima Space Center in Japan abord an H-IIA progress towards its implementation, and plans for archiving and rocket. The instrument is based on a 36-pixel array of distribution of the data. microcalorimeters designed for high resolution over the 0.3-12 keV energy band at the focus of a high throughput, grazing-incidence x-ray mirror. The instrument is the result of a joint collaboration Author(s): Alice Kust Harding1, Zorawar Wadiasingh2 , between the JAXA Institute of Space and Astronautical Science and Christo Venter22 , Markus Boettcher many partners in Japan, and the NASA/Goddard Space Flight Institution(s): 1. NASA's GSFC, 2. North-West University Center and collaborators in the US. The principal components of the spectrometer are the microcalorimeter detector system, a 207.02 – Quasisoft X-ray Sources: their physical low-temperature anticoincidence detector, a 3-stage adiabatic natures revealed demagnetization refrigerator (ADR) to maintain 50 mK operation Quasisoft X-ray sources (QSSs) have been the Mona Lisa of X-ray under both cryogen and cryogen-free operation, a hybrid liquid sources. They have remained enigmatic, even though we have helium/cryogen-free dewar with both Stirling and Joule-Thomson known of their existence and basic properties for more than a coolers, electronics for reading out the array, processing the x-ray decade. QSSs have X-ray luminosities greater than 10^{36} erg/s, data for spectroscopy, and operating the ADR and cryocoolers. The but emit few or no photons above 2 keV. They were discovered in dewar is closed out by an aperture system with five thin-film filters external galaxies during searches for softer sources, supersoft designed to provide high x-ray transmission with low heat loads to X-ray sources (SSSs). Every external galaxy contains QSSs, but it the dewar and detector system, and prevent contamination from has been challenging to find any in the Milky Way and the condensing on the filters. The instrument was designed to have Magellanic Clouds. Recent work, however, reveals that a significant better than 7 eV energy resolution, and was demonstrated to fraction of QSSs may be black holes. We review what is known achieve 4-5 eV resolution across the array at the full spacecraft about QSSs to date, because this obscure class of objects may at last level of integration during extensive ground testing prior to launch. to be ready for "prime time'', capable of identifying BHs in a wide The overall cooling chain has been designed to provide a lifetime of range of Galactic environments. at least 3 years in orbit, and continue to operate without liquid helium to provide redundancy and the longest operational lifetime Author(s): Rosanne Di Stefano1, Francis A. Primini1 , for the instrument. In this presentation, we will describe the early Jincheng Guo12 , Jifeng Liu phases of the SXS instrument in orbit and provide a sense of the Institution(s): 1. Harvard-Smithsonian CfA, 2. National astronomical results that can be expected. Astronomical Observatory of China

This presentation is being given on behalf of the very large 207.03 – Chandra and NuSTAR studies of the international team that developed this complex instrument. ultraluminous X-ray sources in M82 Author(s): Richard L. Kelley2, Kazuhisa Mitsuda1 With the discovery of the ultraluminous X-ray pulsar in M82 by Institution(s): 1. JAXA Institute of Space and Astronautical Bachetti et al (2014), there has been renewed interest in the galaxy, Science, 2. NASA's GSFC which also hosts one of the best candidates for an intermediate-mass black hole. We present results on the spectral 206.03 – ASTRO-H Guest Observer Program and temporal properties of the pulsar from 15 years of Chandra observations with implications for theoretical modeling of the ASTRO-H is a powerful new X-ray observatory for the community: source, as well as the high-energy constraints on both sources from starting approximately 9 month after launch, the bulk of the NuSTAR. observing time will belong to guest observers (GOs) to be allocated via an international Guest Observer program. For US-based Author(s): Murray Brightman1, Fiona Harrison1 , Dom observers, the first call for proposals is a part of ROSES-2016, while Walton31 , Felix Fuerst , Matteo Bachetti 2 , Andreas Zezas 5 , Andrew there are parallel calls for proposals by ESA for European Ptak444 , Ann E. Hornschemeier , Mihoko Yukita , Shriharsh P. astronomers, and by ISAS/JAXA for the Japanese community and Tendulkar11 , Brian Grefenstette all other researchers not in the US or in an ESA member country. Institution(s): 1. California Institute of Technology, 2. INAF/Osservatorio Astronomico di Cagliari, 3. Jet Propulsion We will present the parameters of the Cycle 1 Call for Proposals, Laboratory, 4. NASA Goddard Space Flight Center, 5. University of concentrating on US-specific details as appropriate. We will discuss Crete the international division of observing time, the relationship with the on-going performance verification (PV) phase observations, 207.04 – Probing the clumpy winds of giant stars with our expectation for the number of US targets to be accepted and the high mass X-ray binaries financial support that will be available, and the timeline including the proposal deadline and expected period of Cycle 1 observations Line-driven winds from early type stars are structured, with small, overdense clumps embedded in tenuous hot gas. High mass X-ray Author(s): Koji Mukai2, Robert Petre1 binaries (HMXBs), systems where a neutron star or a black hole Institution(s): 1. NASA/GSFC, 2. UMBC and NASA/GSFC accretes from the line-driven stellar wind of an O/B-type /CRESST companion, are ideal for studying such winds: the wind drives the accretion onto the compact object and thus the X-ray production. The radiation from close to the compact object is quasi-pointlike 207 – Stellar Compact II and effectively X-rays the wind. 207.01 – High-Energy Emission at Shocks in We used RXTE and Chandra-HETG observations of two of the Millisecond Pulsar Binaries brightest HMXBs, Cyg X-1 and Vela X-1, to decipher their wind structure. In Cyg X-1, we show that the orbital variability of A large number of new Black Widow (BW) and Redback (RB) absorption can be only explained by a clumpy wind model and energetic millisecond pulsars have been discovered through radio constrain the porosity of the wind as well as the onion-like searches of unidentified Fermi sources, increasing the known structure of the clumps. In Vela X-1 we show, using the newest number of these systems from 4 to 28. We model the high-energy reference energies for low ionization Si-lines obtained with LLNL’s emission components from particles accelerated to several TeV in EBIT-I, that the ionized phase of the circumstellar medium and the intrabinary shocks in BW and RB systems, and their predicted cold clumps have different velocities. modulation at the binary orbital period. Synchrotron emission is expected at X-ray energies and such modulated emission has Author(s): Victoria Grinberg2, Natalie Hell44 , Maria Hirsch , already been detected by Chandra and XMM. Inverse Compton Javier Garcia12 , David Huenemoerder , Maurice A. Leutenegger 3 , emission from accelerated particles scattering the UV emission Michael Nowak232 , Katja Pottschmidt , Norbert S. Schulz , Jon O. from the radiated companion star is expected in the Fermi and TeV Sundqvists654 , Richard D. Townsend , Joern Wilms bands. Detections or constraints on this emission will probe the Institution(s): 1. Harvard/CfA, 2. Massachusetts Institute of unknown physics of pulsar winds. Technology, Kavli Institute for Astrophysics, 3. NASA/GSFC, 4. Remeis Observatory/ECAP/FAU, 5. Univ. of Wisconsin-Madison, 6. University of Delaware 207.05 – A NICER Look at Accreting Stellar Black simulations. Holes Author(s): Daniel Proga1 We present an overview of NICER’s far-reaching observational Institution(s): 1. Univ. Of Nevada, Las Vegas capabilities for accreting stellar-mass black holes. NICER’s high throughput, large collecting area, and sensitivity at low energies 300.02 – Black holes in the lab: A review of accretion will afford an unprecedented view of black holes across all states. Black hole spectral-timing states are traversed when a black hole experiments using plasmas and liquid metals evolves through its outburst cycle, and each state is comprised of In this talk, we will survey recent liquid metal and plasma thermal disk, Compton, and reflection components. Crucially, experiments attempting to study the magnetorotational instability, NICER will produce our first direct look at oscillations in the and ultimately, turbulent transport of angular momentum in thermal disk itself. Never before has the thermal peak of the laboratory plasmas that can mimic the Keplerian velocity profiles of accretion disk been easily accessible in the time domain. NICER accretion disks. We will describe the basic requirements of such spectra will impose strong constraints on the spectrum of thermal experiments, the techniques used to create such laboratory seed photons and the shape of the Compton component at low experiments, and then review the results obtained thus far. The energies. In addition, NICER will produce reverberation maps of experiments fall into two camps, the first of which use resisitve stellar-mass black holes in each of the thermal, Compton, and Fe-K liquid metal in couette flow geometry, and the second of which (reflection) bands. Such data will be particularly critical for linking uses confined plasma that is stirred by induction on the plasma models of spectral reflection to Comptonization. At the same time, boundary. The regimes covered by liquid metals are compimentary: quasi-periodic X-ray oscillations from the thermal disk may yield liquid metals are very resistive but nearly inviscid and may be precise signatures of a black-hole's spin and would be readily appropriate for modeling protostellar disks, while hot plasmas are detectable with NICER. NICER data will demand a next generation more viscous than resisitve and may be appropriate for hot of self-consistent models and push forward our understanding of accretion disks around black holes. Both approaches have the intricate interplay between Compton, thermal, and reflection overcome major experimental hurdles and now have components. dimensionless parameters that are in a regime where the MRI should be observed. Author(s): James F. Steiner1, Ronald A. Remillard1 Institution(s): 1. MIT Kavli Institute Author(s): Cary Forest1 Institution(s): 1. University of Wisconsin, Madison 207.06 – A Luminous High-Mass Gamma-ray Binary in the Large Magellanic Cloud 300.03 – Recent Observational Progress on Accretion We have been undertaking a search for gamma-ray binaries from Disks Around Compact Objects the detection of periodic modulation in light curves from all Studies of accretion disks around black holes and neutron stars sources in the Fermi LAT 3FGL catalog. From this search we over the last ten years have made remarkable progress. Our identified a 10 day modulation in the direction of the LMC. A understanding of disk evolution as a function of mass accretion localization of the modulation indicates that it arises from a point rate is pushing toward a consensus on thin/thick disk transitions; source identified in a recent Fermi-LAT survey of the LMC. The an apparent switching between disk-driven outflow modes has nature and identification of this source had been uncertain. We emerged; and monitoring observations have revealed complex find that the counterpart is a previously reported candidate spectral energy distributions wherein disk reprocessing must be high-mass X-ray binary with an O6III(f) primary located in a important. Detailed studies of disk winds, in particular, have the supernova remnant. Swift XRT observations of this source show potential to reveal the basic physical processes that mediate disk modulation on the 10 day gamma-ray period, but with a different accretion, and to connect with numerical simulations. This talk will epoch of maximum flux. ATCA radio observations (5.5 and 9 GHz) review these developments and look ahead to the potential of also reveal variable radio emission from this source. Optical Astro-H. spectroscopy (SAAO and SOAR) show that while there are no large 1 changes in the spectrum, there is apparent radial velocity Author(s): Jon M. Miller modulation. At all wavebands this new gamma-ray binary is Institution(s): 1. Univ. of Michigan significantly more luminous than comparable Galactic systems, even though very few of these are known. The discovery of this extragalactic gamma-ray binary may have implications for the 301 – Gravitational Waves overall population of gamma-ray binaries and their evolutionary pathways and lifetimes. 301.01 – Status of Advanced LIGO The two advanced detectors of the Laser Gravitational Wave Author(s): Robin Corbet9, Chi C. Cheung64 , Laura Chomiuk , Observatory (LIGO) recently completed their first Observing run Malcolm J. Coe75 , Joel Barry Coley , Guillaume Dubus 2 , Philip O1. Targeting a factor of 10 sensitivity improvement over initial Edwards13 , Pierrick Martin , Vanessa McBride 81 , Jamie Stevens , detectors, Advanced LIGO promises to open the new era of Jay Strader48 , Lee Townsend gravitational wave astronomy. Even if not yet operating at full Institution(s): 1. CSIRO, 2. Grenoble , 3. IRAP, 4. MSU, 5. NASA sensitivity, with O1 Advanced LIGO has already largely surpassed GSFC, 6. NRL, 7. Southampton University, 8. UCT, 9. UMBC the space-time volume surveyed by previous observations. This talk describes the Advanced LIGO detectors, their current sensitivity performance, and future prospects.

300 – The Physics of Accretion Disks – A Author(s): Lisa Barsotti1 Joint HEAD/LAD Session Institution(s): 1. MIT

300.01 – The theory of accretion disks - insights from 301.02 – Fermi GBM Counterparts to LIGO local and global simulations Gravitational-Wave Candidates In this brief review, I summarize the key physical processes that are As the advanced configuration of the Laser Interferometer believed to operate in accretion disks. To understand each of these Gravitational-wave Observatory has begun operations, we eagerly processes, e.g., the angular transport that is facilitated by the anticipate the detection of gravitational waves (GW) with LIGO in so-called magneto-rotational instability or large scale outflow, as coincidence with a gamma-ray signal from the Fermi Gamma-ray well as their interplay, one has to use numerical simulations Burst Monitor (GBM). The most likely source is a short to gain insights into the time-dependent, multi-dimensional and Gamma-Ray Burst (GRB) arising from the merger of two compact -scale nature of accretion disks. Therefore, I also objects. With its broad sky coverage, GBM triggers and localizes present some results of most recent local and global numerical more short GRBs than other active space missions, ~40 each year. Combining GBM and LIGO localization uncertainty regions may inspirals to compact galactic binary systems. provide a smaller target to look for the GW host. A joint GBM-LIGO The L3 mission is expected to be based on the eLISA/LISA design detection increases the confidence in the GW detection and helps which was submitted by the eLISA consortium as a notional characterize the parameters of the merger. Offline searches for mission concept. NASA started discussions with ESA how to join weak GRBs that fail to trigger onboard Fermi indicate that L3 and participates in ESA’s Gravitational Observatory Advisory additional short GRBs can be detected in the GBM data. I will Team. NASA is also in the process of setting up its own L3-Study discuss the implementation and expected benefits of joint searches team to look at potential US contributions to L3. This group will to detect and localize GW candidates. I will also explore how the also act as the US partner for the eLISA consortium. In summary, non-detection in the GBM data of a signal consistent with GW the space component of the GW community has gained significant candidates in the LIGO data can affect follow-up strategies for momentum over the last 12 months and a successful pathfinder counterpart searches by other observers. mission and potential GW discoveries by Advanced LIGO and/or pulsar timing arrays should further strengthen the case for LISA. Author(s): Eric Burns5, Lindy Blackburn2 , Michael Stephen Briggs53 , Jordan Camp , Nelson Christensen 1 , Valerie Author(s): Guido Mueller1 Connaughton84 , Adam Goldstein , Tyson Littenberg 8 , Judith L. Institution(s): 1. University of Florida Racusin37 , Peter S. Shawhan , Leo Pound Singer 36 , John Veitch , Binbin Zhang5 Institution(s): 1. Carleton College, 2. Harvard–Smithsonian 302 – Missions & Instruments Center for Astrophysics, 3. NASA/GSFC, 4. NASA/MSFC, 5. University of Alabama in Huntsville, 6. University of Birmingham, 302.01 – NICER: Mission Overview and Status 7. University of Maryland, 8. USRA NASA's Neutron star Interior Composition Explorer (NICER) mission will explore the structure, dynamics, and energetics of 301.03 – LISA Pathfinder and the road to space-based neutron stars through soft X-ray (0.2–12 keV) timing and detection of gravitational waves spectroscopy. An external attached payload on the International The LISA Pathfinder spacecraft was launched on Dec 3rd, 2015 and Space Station (ISS), NICER is manifested on the Commercial began science operations in March 2016. Led by the European Resupply Services SpaceX-11 flight, with launch scheduled for late Space Agency with contributions from a number of European 2016. The NICER payload is currently in final integration and national agencies, universities, and NASA, LISA Pathfinder will environmental testing. Ground calibration has provided robust demonstrate several key technologies and measurement performance measures of the optical and detector subsystems, technqiues for future space-based gravitational wave observatories. demonstrating that the instrument meets or surpasses its effective A successful LISA Pathfinder will retire much of the technical risk area, timing resolution, energy resolution, etc., requirements. We for such missions, which are the only proposed instruments briefly describe the NICER hardware, its continuing testing, capable of observing gravitational waves in the milliHertz band, a operations and environment on ISS, and the objectives of NICER's source-rich region expected to include singals from merging prime mission—including precise radius measurements for a extragalactic massive black holes, capture of stellar-mass compact handful of neutron stars to constrain the equation of state of cold, objects by massive black holes, and millions of individual close ultra-dense matter. Other contributions at this meeting address compact binaries in the Milky Way. I will present an overview of specific scientific investigations that are enabled by NICER, for the LISA Pathfinder mission, it's current status, and the plans for neutron stars in their diverse manifestations as well as for broader operations and data analysis. X-ray astrophysics through a brief, approved Guest Observer program beginning in 2018. Author(s): James Thorpe1 Institution(s): 1. NASA GSFC Author(s): Zaven Arzoumanian2, Keith C. Gendreau1 Institution(s): 1. NASA/GSFC, 2. Universities Space Research 301.04 – Bringing Black Holes Together: How Association Supermassive Black Hole Binaries Form and Plunge Through the Final Parsec 302.02 – Observatory Science with the NICER X-ray Timing Instrument This presentation is submitted on behalf of the NICER Observatory Astronomers now know that supermassive black holes reside in Science Working Group. NICER will be deployed on the nearly every galaxy. International Space Station later in 2016. The X-ray sensitivity Though these black holes are an observational certainty, nearly spans 0.2-12 keV, with CCD-like spectral resolution, low every aspect of their evolution -- from their birth, to their fuel background rates, and unprecedented timing accuracy. A Guest source, to their basic dynamics -- is a matter of lively debate. In Observer (GO) Program has been approved by NASA as one of the principle, gas-rich major galaxy mergers can generate the central proposed Science Enhancement Options, contingent on NICER stockpile of fuel needed for a low mass central black hole seed to meeting its Prime Mission Science Objectives. The NICER Science grow quickly into a supermassive one. During a galaxy merger, the team will observe limited Observatory Science targets (i.e., sources black holes in each galaxy meet and form a supermassive binary other than neutron stars) in year 1, and GO observations will black hole; as the binary orbit shrinks through its final parsec, it constitute 50% of the exposures in year 2. Thereafter, NICER will becomes the loudest gravitational wave source in the Universe and compete for continuation via the NASA Senior Review process. a powerful agent to sculpt the galactic center. This talk will touch NICER Instrument performance is compared with Missions such on some current and ongoing work on refining our theories of how as XMM-Newton and RXTE. We briefly highlight the expected supermassive black hole binaries form, evolve within, and alter themes for Observatory Science relating to accreting black holes on their galaxy host. all mass scales, magnetic CVs, active stars, and clusters of galaxies.

Author(s): Kelly Holley-Bockelmann1 Author(s): Ronald A. Remillard1 Institution(s): 1. Vanderbilt University Institution(s): 1. MIT

301.05 – ESA’s L3 mission: A space-based 302.03 – Arcus: Exploring the Formation and gravitational-wave observatory Evolution of Clusters, Galaxies, and Stars ESA selected the Gravitational Universe as the science theme for We present the scientific motivation and performance for Arcus, an one of its future L-class missions. L3 will measure gravitational X-ray grating spectrometer mission to be proposed to NASA as a waves in the 10µHz to 100mHz window; probably the richest of all MIDEX in 2016. This mission will observe structure formation at gravitational wave windows. Expected sources in this frequency and beyond the edges of clusters and galaxies, feedback from band range from massive black hole mergers to extreme mass ratio supermassive black holes, the structure of the interstellar medium and the formation and evolution of stars. Key mission design (LOFT-P): A Probe-Class Mission Concept parameters are R = 3000 with >500 cm2 of effective area at the LOFT-P is a mission concept for a NASA Astrophysics Probe-Class crucial O VII and O VIII lines, with the full bandpass going from (<$1B) X-ray timing mission, based on the LOFT M-class concept ~10-50 Angstroms. Arcus will use the silicon pore optics developed originally proposed to ESA’s M3 and M4 calls. LOFT-P requires for ESA’s Athena mission, paired with off-plane gratings being very large collecting area, high time resolution, good spectral developed at the University of Iowa and combined with resolution,broadband spectral coverage (2-30 keV), highly flexible MIT/Lincoln Labs CCDs. With essentially no consumables, Arcus scheduling, and an ability to detect and respond promptly to should achieve its mission goals in under 2 years, after which we time-critical targets of opportunity. It addresses science questions anticipate a substantial period of operation as a general such as: What is the equation of state of ultra dense matter? What observatory. are the effects of strong gravity on matter spiraling into black 1 holes? It would be optimized for sub-millisecond timing of bright Author(s): Randall K. Smith Galactic X-ray sources including X-ray bursters, black hole Institution(s): 1. Smithsonian Astrophysical Observatory binaries, and magnetars to study phenomena at the natural timescales of neutron star surfaces and black hole event horizons 302.04 – MeV Science with the Advanced Energetic and to measure mass and spin of black holes. These measurements Pair Telescope (AdEPT), a High Sensitivity Medium- are synergistic to imaging and high-resolution spectroscopy Energy Gamma-Ray Polarimeter instruments, addressing much smaller distance scales than are Many high-energy astrophysical phenomena exhibit unique, possible without very long baseline X-ray interferometry, and using transitory behavior, such as spectral breaks, bursts, and flares complementary techniques to address the geometry and dynamics below ~200 MeV. However, while significant progress in of emission regions. LOFT-P would have an effective area of >6 gamma-rays has been made by instruments such as Fermi and m2 , >10x that of the highly successful Rossi X-ray Timing Explorer AGILE, a significant sensitivity gap remains in the medium-energy (RXTE). A sky monitor (~2-50 keV) acts as a trigger for pointed regime (0.75 - 200 MeV) that has been explored only by COMPTEL observations, providing high duty cycle, high time resolution and EGRET on CGRO. Tapping into this unexplored regime monitoring of the X-ray sky with ~20 times the sensitivity of the requires development of a telescope with significant improvement RXTE All-Sky Monitor, enabling multi-wavelength and multi- in sensitivity. Our mission concept, covering ~5 to ~200 MeV, is messenger studies. A probe-class mission concept would employ the Advanced Energetic Pair Telescope (AdEPT). The AdEPT lightweight collimator technology and large-area solid-state telescope will achieve angular resolution of ~0.6 deg at 70 MeV, detectors, segmented into pixels or strips, technologies which have similar to the angular resolution of Fermi/LAT at ~1 GeV that been recently greatly advanced during the ESA M-3 Phase A study brought tremendous success in identifying new sources. AdEPT of LOFT. Given the large community interested in LOFT (>800 will also provide unprecedented polarization sensitivity, ~1% for a 1 supporters), the scientific productivity of this mission is expected to Crab source. The enabling technology for AdEPT is the Three- be very high, similar to or greater than RXTE (~2000 refereed Dimensional Track Imager (3-DTI) a low-density, large volume, gas publications.) In May 2016, MSFC’s Advanced Concepts Office will time-projection chamber with a 2-dimensional readout. The 3-DTI perform a study of a US-led probe-class LOFT concept. This is provides high-resolution three-dimensional electron tracking with presented on behalf of the LOFT consortium. minimal Coulomb scattering that is essential to achieve high angular resolution and polarization sensitivity. We describe the Author(s): Colleen A. Wilson-Hodge3, Paul S. Ray4 , Deepto design, fabrication, and performance of the 3-DTI detector, Chakrabarty21 , Marco Feroci describe the development of a 50x50x100 cm3 AdEPT prototype, Institution(s): 1. INAF-IAPS, 2. MIT, 3. NASA/MSFC, 4. NRL and highlight a few of the key science questions that AdEPT will address. 303 – Mid-Career Prize Talk: In the Ring Author(s): Tonia M. Venters1, Stanley D. Hunter1 , Georgia De Nolfo11 , Andrei R Hanu , John F Krizmanic 1 , Floyd W. Stecker 1 , with Circinus X-1: A Three-Round Struggle to Andrey Timokhin1 Reveal its Secrets, Sebastian Heinz (Univ. of Institution(s): 1. Goddard Space Flight Center Wisconsin) 302.05 – AdEPT, the Advanced Energetic Pair 303.01 – In the Ring with Circinus X-1: A Three-Round Telescope for Medium-Energy Gamma-Ray Struggle to Reveal its Secrets Polarimetry I will discuss the science of X-ray light echoes from Galactic X-ray The Advanced Energetic Pair Telescope (AdEPT) is being transients. When a bright transient flare is affected by a sufficiently developed as a future NASA/GSFC end-to-end MIDEX mission to high column of interstellar dust (N_H ~10^22 cm^-2), the perform high-sensitivity medium-energy (5–200 MeV) astronomy scattered X-ray echo from the flare can take the form of and revolutionary gamma-ray polarization measurements. The well-defined rings. Resolved X-ray imaging of the rings allows us to enabling technology for AdEPT is the GSFC Three-Dimensional construct sensitive probes of the dust mass distribution along the Track Imager (3-DTI), a large volume gaseous time projection line of sight, to constrain dust properties like dust composition and chamber with 2-dimentional micro-well detector (MWD) readout. grain size distributions, and to measure the distance to the X-ray The low density and high spatial resolution of the 3-DTI allows source. With only three well-documented echoes reported to date, AdEPT to achieve high angular resolution (~0.5 deg at 67.5 MeV) this is a relatively new field of study with a bright future. I will and, for the first time, exceptional gamma-ray polarization briefly touch on the requirements for future X-ray missions to sensitivity. These capabilities enable a wide range of scientific advance the study of X-ray echoes. discovery potential for AdEPT. We will discuss several of the key science goals of the AdEPT mission. These include: 1) Explore Author(s): Sebastian Heinz1 fundamental processes of particle acceleration in active Institution(s): 1. Univ. Of Wisconsin, Madison astrophysical objects, 2) Reveal the magnetic field configuration of the most energetic accelerators in the Universe, 3) Explore the origins and acceleration of cosmic rays and the Galactic MeV diffuse emission, 4) Search for dark matter in the Galactic center, 304 – Science of X-ray Polarimetry in the and 5) Test relativity with polarization measurements. 21st Century Author(s): Stanley D. Hunter1 304.01 – The Scientific Potential of X-ray Polarimetry Institution(s): 1. NASA/GSFC X-ray Polarimetry is a rich, untapped source of information on the geometry and/or magnetic structure of a wide range of cosmic 302.06 – Large Observatory For X-ray Timing object from accreting black holes to jets and neutron stars. This introductory overview will outline the basics of the production of X-ray synchrotron radiation traces the high energy extrema of polarized X-ray emission and emphasise its importance in our e+/e- accelerated by pulsar magnetospheres and supernova quest to understand how compact objects work. shocks. X-ray polarization lets us probe the unresolved geometry of these relativistic shock structures. I summarize what we know Author(s): Andrew C Fabian1 about magnetic field geometries in these nebulae and the prospects Institution(s): 1. University of Cambridge for learning more from X-ray polarimetry.

304.02 – X-ray polarimetric studies of stellar mass Author(s): Roger W. Romani1 black holes Institution(s): 1. Stanford Univ. Stellar mass black holes are among the brightest X-ray sources in the sky. Thus, they are excellent candidates for X-ray polarimetry, a technique that requires very large number of photons for a 305 – Making the Multimessenger – EM sensitive measurement. For accreting black holes in the thermal state, polarization provides important information about the black Connection hole's spin magnitude and orientation relative to the observer. For black holes in the "low-hard" or "steep power-law" states, 306 – SNR/GRB/Gravitational Waves polarization provides a unique probe of the geometry of the hot electron corona. 306.01 – The 3D Distribution of 44-Ti in Cassiopeia A 1 The mechanisms behind core-collapse supernovae represent one Author(s): Jeremy Schnittman of the most important unsolved problems in stellar astrophysics Institution(s): 1. NASA/GSFC and are of interest to many branches of physics and astronomy, such as nucleosynthesis, pulsar formation, gamma-ray bursts, and 304.03 – Scientific Drivers for X-Ray Polarimetry gravitational wave production. Few direct observational constraints Observations of Active Galactic Nuclei and Blazars exist that probe fundamental parameters such as the explosion Spectropolarimetric observations promise to give us insights into asymmetries and dynamics. One of the most direct probes of the the structure of the the accretion flows and collimated outflows physics of the core-collapse supernova engine is 44 Ti, which is (jets) of mass accreting supermassive black holes. In this talk, I will producing near the "mass cut" in the collapsing star with material present results from general relativistic ray tracing studies showing interior to the 44 Ti accreting onto the nascent compact object the that the spectropolarimetric observations of bright Seyfert galaxies the 44 Ti mostly ejected during the explosion. give information that is complimentary to that from Fe K-alpha line and Compton reflection hump spectroscopy. Combining Here we present the results from the full NuSTAR observational polarimetric with spectral and timing results will allow us to pin campaign (over 2 Ms) of the famous Type II supernova remnant down the physical properties of the accretion disk and corona with Cassiopeia A (Cas A). NuSTAR is the first X-ray observatory higher accuracy and with smaller systematic uncertainties. The capable of focusing the X-rays that are emitted during the X-ray polarimetric observations of blazars (mass accreting radioactive decay of 44 Ti to 44 Ca. For a supernova remnant like supermassive black holes with jets aligned with the line of sight) Cas A, which is both young and nearby, we can to image the will allow us to study the structure of the magnetic field inside the distribution of the 44 Ti ejecta. Early results (using the first 1 Ms of jets (and thus to constrain the jet launching mechanism) in high data) produced the first 2D maps of the 44 Ti in Cas A, revealing the synchrotron peaked blazars, and to identify and constrain the asymmetry in the 44 Ti ejecta and the striking discrepancy between emission mechanism responsible for the X-ray to gamma-ray the distributions of 44 Ti and the ionized Fe emission seen by emission in low and intermediate synchrotron peaked blazars. Chandra. With the additional exposure time we can perform spatially-resolved spectroscopy to determine the Doppler shift of Author(s): Banafsheh Beheshtipour1 the 44 Ti-emitting regions, giving us the ability to construct a 3D Institution(s): 1. Washington University in St. Louis representation of the remnant. We can compare this to the excellent data from Chandra and Spitzer which have been used to 304.05 – Probes of Fundamental Physics using X-ray perform similar studies of the ionized X-ray ejecta and IR emitting Polarimetry ejecta, respectively. We find an increasingly complex picture of the The advent of X-ray polarimetry as an astronomical discipline is on remnant, with 44 Ti appearing wtih Fe in some regions on the the near horizon. Prospects of Explorer class missions currently remnant and other regions of Fe that are apparently 44 Ti free. We under study in the NASA SMEX program, the Xipe mission under will discuss our findings, and the implications of these results. ESA study in Europe, and beyond to initiatives under development 1 4 in Asia, indicate that the worldwide high energy astrophysics Author(s): Brian Grefenstette , Steven E. Boggs , Chris 211 1 community view this as a high priority. The focal goal of X-ray Fryer , Fiona Harrison , Kristin Madsen , Hiromasa Miyasaka , 34 polarization measurements is often to discern the geometry of a Stephen P. Reynolds , Andreas Zoglauer source, for example an accreting black hole, pulsing neutron star or Institution(s): 1. Caltech, 2. Los Alamos National Laboratory, 3. a relativistic jet; these are addressed in other talks in this HEAD NC State, 4. Space Sciences Laboratory special session. In this talk, I discuss a parallel agenda, to employ X-ray polarimetry to glean insights into fundamental physics that is 306.02 – G346.6-0.2: A Rare Mixed-Morphology presently difficult or impossible to test in laboratory settings. Much Supernova Remnant with Non-Thermal X-Ray of this is centered around neutron stars, and I will Emission address theoretically-expected signatures of vacuum birefringence The detection of non-thermal X-ray emission from supernova and photon splitting, predictions of QED theory in the strong remnants (SNRs) provides us with a unique window into studying magnetic fields possessed by pulsars and magnetars. Of particular particle acceleration at the shock-front of an SNR. All of the 14 or note is that time-dependent polarimetry coupled with spectroscopy so SNRs in which non-thermal X-ray synchrotron emission has can help disentangle purely geometrical effects and fundamental been detected are shell-like in nature, and show no evidence of physics ones. A brief discussion of possible tests of Lorentz interaction with large nearby molecular clouds. Here we present a invariance violation, expected in some theories of quantum gravity, new X-ray study of the molecular cloud interacting mixed- will also be presented. Instrument requirements to realize such morphology SNR G346.6-0.2 using XMM-Newton. We found that science goals will also be briefly covered. the X-ray emission arises from a cool recombining plasma with subsolar abundance, confirming previous Suzaku results. In Author(s): Matthew G. Baring1 addition, we identified an additional power-law component in the Institution(s): 1. Rice University spectrum, with a photon index of ~2. We investigated its possible origin and conclude that this is most likely synchrotron emission 304.06 – X-ray Polarization Probes of SNR and PWN produced by particles accelerated at the shock. We also derive the age of the remnant to be 1.8-2.3 kyrs assuming a distance of 8.3 Author(s): Kenji Hamaguchi2, Michael F. Corcoran2 , Neetika kpc, which is much younger than previously suggested, while based Sharma11 , Theodore R. Gull 6 , Hiromitsu Takahashi 5 , Brian on its morphology, Galactic location and the density of its Grefenstette17 , Takayuki Yuasa , Martin Stuhlinger 3 , Christopher environment as derived from our X-ray analysis, the progenitor of Michael Post Russell692 , Anthony F. J. Moffat , Thomas Madura , G346.6-0.2 was most likely a massive star. Noel Richardson12 , Jose Groh 4 , Julian Pittard 8 , Stan Owocki 10 Institution(s): 1. California Institute of Technology, 2. CRESST Author(s): Katie Amanda Auchettl2, B.T.T. Wong3 , Chi Yung NASA's GSFC, 3. European Space Astronomy Centre, 4. Geneva Ng31 , Patrick O. Slane University, 5. Hiroshima University, 6. NASA's GSFC, 7. RIKEN, Institution(s): 1. Harvard-Smithsonian, CfA, 2. The Ohio State 8. The University of Leeds, 9. Universite de Montreal, 10. University, 3. The University of Hong Kong University of Delaware, 11. University of Maryland, Baltimore County, 12. University of Toredo 306.03 – Galactic Astrophysics at TeV: One Year of Observations with HAWC 306.05 – Mergers of Binary Neutron Star Systems The High-Altitude Water Cherenkov Gamma Ray Observatory, or We present results from fully relativistic simulations of binary HAWC, is joint US/Mexican air shower array designed to observe neutron star mergers varying the tabular equation of state used to gamma rays and cosmic rays between 100 GeV and 100 TeV. approximate the degenerate material and the mass ratio. The HAWC is currently the only high-uptime wide-field TeV simulations incorporate both magnetic fields and the effects of observatory in operation. The observatory is carrying out an neutrino cooling. In particular, we examine the amount and unbiased survey of the Northern Hemisphere, has a robust properties of material ejected from the merger. We gratefully program to search for flares and other transient sources of gamma acknowledge the support of NASA through the Astrophysics rays, and is well suited to observe spatially extended regions of Theory Program grant NNX13AH01G. gamma-ray emission and cosmic-ray anisotropy. HAWC recently concluded its first year of data taking with the complete array. The Author(s): Patrick M. Motl3, Matthew Anderson2 , Luis results include not only observations of many known TeV point Lehner541 , Steven Liebling , David Neilsen , Carlos Palenzuela 6 sources, but also extended emission from Galactic objects like the Institution(s): 1. Brigham Young University, 2. Indiana Geminga supernova remnant. These results have implications for University, 3. Indiana University Kokomo, 4. Long Island the origins of several astrophysical anomalies observed in the University, 5. Perimeter Institute for Theoretical Physics, 6. cosmic-ray data, such as the excess of Galactic positrons at Earth. Universitat de les Illes Ballears We will describe results from HAWC with a focus on the observation of cosmic rays and Galactic sources of gamma rays. 306.06 – Broadband Electromagnetic Follow-up of Advanced LIGO Sources 1 Author(s): Segev BenZvi Advanced LIGO began observing in September 2015 with over 3 Institution(s): 1. University of Rochester times the distance reach (27 times the sensitive volume) of its previous configuration. Some gravitational-wave sources, 306.04 – Eta Carinae's Hard X-ray Tail Measured with particularly neutron star binary mergers, are expected to produce XMM-Newton and NuSTAR broadband electromagnetic transients which may be crucial to Massive binary stellar systems drive shock plasma heating via the understanding the astrophysical context of these events. We have collision of winds from two stars (wind-wind collision: WWC). assembled a consortium of over 60 ground- and space-based With typical (pre-shock) wind speeds of ≥1000 km s-1 , gamma-ray, x-ray, optical, infrared, and radio facilities temperatures can reach as high as several tens of millions of collaborating to search for broadband electromagnetic counterparts Kelvin. X-ray emission from these stable shocks provides of gravitational-wave sources. In this talk, we describe the important tests of shock physics. While the spectrum below 10 keV LIGO/Virgo EM follow-up program and the astronomical facilities is complicated by discrete line emission and absorption that participated during this first LIGO observing run. Then, we components, the X-ray spectrum above 10 keV is relatively simple. survey the multi-wavelength observing campaigns embarked upon This high-energy emission therefore provides important clues on for specific gravitational-wave events. Finally, we discuss lessons the condition of the maximum thermalized plasma where the learned and the way forward for joint GW-EM observations in an winds collide head-on, while also providing important information era of increasingly sensitive GW detectors. about particle acceleration through the shock. Submitted with The LIGO Scientific Collaboration and The Virgo We obtained two coordinated X-ray observations of the super Collaboration. massive binary system η Carinae with XMM-Newton and NuSTAR, during the elevated X-ray flux state and just before the X-ray Author(s): Leo Pound Singer1 minimum flux state around the periastron passage in the summer Institution(s): 1. NASA Goddard Space Flight Center of 2014. These NuSTAR observations clearly detected X-ray emission associated with η Car extending up to ~50 keV for the 306.07 – Estimating Long GRB Jet Opening Angles first time. The NuSTAR spectrum above 10 keV can be fit with the and Rest-Frame Energetics bremsstrahlung tail from a kT ~6 keV plasma, about 2 keV higher We present a method to estimate the jet opening angles of long than those measured from the iron K emission line complex. This duration Gamma-Ray Bursts (GRBs) using the prompt gamma-ray result may suggest that the companion star's pre-shock wind energetics and a correlation between the time-integrated peak velocity is underestimated. The NuSTAR observation near the energy of the GRB prompt spectrum and the collimation-corrected X-ray minimum state showed a gradual decline in the >5 keV energy in gamma rays. The derived jet opening angles using this emission by 40% in a day. The extreme absorption to the hardest method match well with the corresponding inferred jet opening emission component (NH~1e24 cm-2 ) suggests increased angles obtained when a break in the afterglow is observed. obscuration of the WWC X-ray emission by the thick primary Furthermore, using a model of the predicted long GRB redshift stellar wind prior to superior conjunction. Neither observation probability distribution observable by the Fermi Gamma-ray Burst detected the power-law component in the extremely hard band that Monitor (GBM), we estimate the probability distributions for the INTEGRAL and Suzaku observed prior to 2011. If the jet opening angle and rest-frame energetics for a large sample of non-detection by NuSTAR is caused by absorption, the power-law GBM GRBs for which the redshifts have not been observed. source must be small and located very near the WWC apex. Previous studies have only used a handful of GRBs to estimate Alternatively, it may be that the power-law source is not related to these properties due to the paucity of observed afterglow jet breaks, either η Car or the GeV gamma-ray source. spectroscopic redshifts, and comprehensive prompt gamma-ray observations, and we expand the number of GRBs that can be used We also introduce the result of the latest XMM-Newton and in this analysis by more than an order of magnitude. In this NuSTAR joint observation of η Car performed in 2015 July. analysis, we also present an inferred distribution of jet breaks which indicates that a large fraction of jet breaks are not observable related to properties and evolution of AGN call for more sensitive with current instrumentation and observing strategies. We present surveys rather than larger numbers of AGN. To address these simple parameterizations for the jet angle, energetics, and jet break issues we have developed a new survey technique by merging the distributions so that they may be used in future studies. independent observations of BAT and IBIS/ISGRI: the Swift- INTEGRAL X-ray (SIX) survey. This survey capitalizes on the very Author(s): Adam Goldstein1, Valerie Connaughton3 , Michael uniform BAT sensitivity over the entire sky and the very deep Stephen Briggs22 , Eric Burns sensitivity of IBIS/ISGRI over selected sky areas. Institution(s): 1. NASA Postdoctoral Program, 2. Univ. of We present the SIX survey technique and its results in terms of Alabama in Huntsville, 3. USRA properties and evolution of AGN in the local Universe. Finally we will show our predictions and simulations for an approved 9 Ms 306.08 – Strong constraints on gamma-ray burst survey performed by INTEGRAL/IBIS on a selected sky area. This emission in TeV using recent results from VERITAS will allow us to build with the SIX a reference sample of AGN in the Recent VERITAS gamma-ray upper limits in the energy range 100 local Universe in terms of redshift – luminosity parameter space. GeV to 30 TeV suggest that gamma-ray burst (GRB) emission in We discuss this in the context of the NuSTAR survey. TeV is substantially suppressed compared to X-ray emission, and 1 even compared to typically-observed Fermi-LAT emission in GeV. Author(s): Eugenio Bottacini These results impact on our understanding of the GRB Institution(s): 1. Stanford University environment. We will present VERITAS results on GRB150323A and put them in context of what has been seen at lower energies by 400.04 – Circumnuclear Star Formation in the BAT Swift and Fermi, both for this particular burst and for others. AGN Sample: High Resolution Radio Morphologies and SFRs Author(s): Ori Weiner1 It has long been an assumption that active galaxies would obey the Institution(s): 1. Columbia University same far-infrared (FIR) - radio correlation established for star-forming normal galaxies. This assumption has been used by numerous high-z studies, but has recently come into doubt for two 400 – AGN II main reasons: the revelation that the AGN itself may contribute non-negligibly to the FIR emission, and different radio emission 400.01 – Resolving the Cosmic X-ray Background with physics in the vicinity of the active nucleus than in isolated HII NuSTAR and Chandra regions. Studies have attempted to decompose the FIR spectral Although its origin was long mysterious, the cosmic X-ray energy distributions to remove the AGN contribution and then background (CXB) is now known to be primarily the sum of calculate the star formation rate (SFR). It would then be ideal to emission from large number of active galactic nuclei (AGN). With compare this to another, independent measure of SFR. We have the advent of NuSTAR, the first focusing high-energy X-ray conducted a high-resolution (0.3-1'') JVLA survey of an unbiased observatory, we can now directly identify the sources that sample of nearby, hard X-ray selected AGN in order to spatially contribute to the bulk of the CXB at energies > 10 keV where the decompose the extended star formation emission from the central CXB spectrum peaks. I will present an analysis using data from the compact source. We present these maps of the nuclear regions of NuSTAR extragalactic survey program in which we using stacking 41 AGN from the Swift-BAT sample. The objects exhibit a wide techniques to determine the fraction of the CXB that is produced range of circumnuclear radio morphologies, including mini-jets by X-ray sources identified at softer energies by deep Chandra and star-forming rings. When the central compact source is observations. These results provide important constraints on AGN removed, the extended emission does indeed conform to the synthesis models fo the CXB and point toward a further "missing" FIR-radio correlation. A subset of the objects also remain compact population of obscured AGN. This work is supported in part by in our 1'' and 0.3'' observations, implying very high star formation NASA award NNX15AP24G. surface densities which may be capable of driving significant winds.

Author(s): Ryan C. Hickox1 Author(s): Krista Lynne Smith2, Richard Mushotzky2 , Stuart Institution(s): 1. Dartmouth College N. Vogel21 , Neal A. Miller Institution(s): 1. Stevenson University, 2. University of 400.02 – Looking for early black holes signatures in Maryland College Park the anisotropies of Cosmic backgrounds We currently do not know how Super Massive Black Holes are 400.05 – Testing the CMB Quenching for seeded and grow to form the observed massive QSO at z~7. This is High-Redshift Radio Galaxies puzzling, because at that redshift the Universe was still too young The identification of a dozen of high-redshift (z > 4) blazars implies to allow the growth of such massive black holes from stellar that a much larger population of powerful, but mis-aligned jetted remnant black hole seeds. Theoretical models, taking into account AGNs already exists in the early Universe. However, this parent the paucity of metals in the early Universe, explain this by invoking population remains elusive, although they are expected to be the formation of massive black holes seeds at z>10 as Direct within the sensitivity threshold of modern wide-field radio surveys. Collapse Black holes of remnants of dead POPIII stars. As of today One appealing mechanism is that the CMB photons upscatter the we cannot claim any detection of any high-z (z>7) black hole in diffuse synchrotron radio emission in the lobes to the X-ray band. their early stage of life. However, our recent measures of the In this scenario, the lobes will turn into luminous X-ray sources. arcminute scale joint fluctuations of the Cosmic X-ray Background We analyzed the extended X-ray emission around several radio and the Cosmic Infrared Background by Chandra and Spitzer can galaxies at z~4 and constructed their broad-band spectral energy be explained by a population of highly absorbed z>10 Direct distributions (SEDs). Modeling their SEDs will test this CMB Collapse Black Holes. quenching scenario for high-redshift radio galaxies. I will review the recent discoveries obtained with different instruments and by different teams and critically discuss these Author(s): Jianfeng Wu1, Elena Gallo1 findings and the interpretations. Institution(s): 1. University of Michigan

Author(s): Nico Cappelluti1 400.06 – Can Supermassive Black Holes Influence the Institution(s): 1. Yale University Evolution of their Host Galaxies? Powerful winds driven by active galactic nuclei (AGN) are often 400.03 – Deeply X-raying the Local Universe invoked to play a fundamental role in the evolution of both Swift/BAT and INTEGRAL/IBIS have revolutionized our view of supermassive black holes (SMBHs) and their host galaxies, Active Galactic Nuclei (AGN) in the local Universe. Their successful quenching star formation and explaining the tight SMBH-galaxy ongoing surveys count hundreds of AGN. However essential issues relations. A strong support of this "quasar-mode" feedback came from the recent X-ray observation of a mildly relativistic accretion disk wind in the ultraluminous infrared galaxy IRAS F11119+3257 This research is supported in part by NASA through Swift Guest hosting a luminous quasar at the center. Energetics arguments Investigator grants NNX15AR45G and NNX15AR34G. indicate a connection with a massive, large-scale molecular outflow observed in infrared with Herschel. This seems to be in agreement Author(s): Alan P. Marscher1, Svetlana G. Jorstad1 with theoretical models in which AGN winds drive hot bubbles in Institution(s): 1. Boston Univ. the host galaxy medium, thereby providing a link between the SMBH and the gas out of which stars form. This work was the 401.04 – Using the Long-term Optical/Infrared Color “cover story” of the March 26th 2015 issue of Nature. Variability to Trace the Gamma-ray Jet "State" Revolutionary improvements in this field are expected from We have undertaken a 7-year, multiwavelength program to observe ASTRO-H and Athena. a sample of blazars in various Fermi gamma-ray states, using the Small and Medium Aperture Research Telescope System Author(s): Francesco Tombesi2, Sylvain Veilleux3 , James 13 (SMARTS) 1.3m + ANDICAM instrument in Cerro Tololo, Chile. Reeves , Christopher S. Reynolds We present near-daily optical and infrared (OIR) color variability Institution(s): 1. Keele University , 2. NASA/GSFC, 3. University diagrams of these sources and compare the OIR flux and color to of Maryland the Fermi gamma-ray flux on similar cadence. We then analyze the color variability properties on short and long timescales, as compared to the length of an average gamma-ray flare, to better 401 – The Unique Role of Very High Energy constrain the physical mechanisms responsible for the variability properties that we observe. From this long-term observational data, Observations in Multi-Wavelength we develop a schematic representation of the possible color Astronomy variability behaviors in blazars and how it is related to the thermal disk and non-thermal jet contributions in both Flat Spectrum 401.01 – Very-High-Energy Astrophysics with the Radio Quasars and BL Lac objects. Cherenkov Telescope Array The Cherenkov Telescope Array (CTA) will be a new gamma-ray Author(s): Jedidah Isler1, C. Megan Urry22 , Charles D. Bailyn , observatory in the energy band ~30 GeV to ~100 TeV, designed to Paolo S. Coppi22 , Imran Hasan , Emily MacPherson 2 , Michelle achieve an order of magnitude improvement in sensitivity over the Buxton2 currently operating imaging atmospheric Cherenkov telescopes. Institution(s): 1. Vanderbilt University, 2. Yale University CTA will probe known sources with unprecedented sensitivity, angular resolution, and spectral coverage, with the potential of 401.05 – Mapping supernova remnants and pulsar detecting hundreds of new sources. The CTA Consortium will also wind nebulae across decades of energy conduct a number of Key Science Projects, including a Galactic Ground- and space-based gamma ray observatories of the past Plane survey and a survey of one quarter of the extragalactic sky. decade have given us a new understanding of particle accelerators Data taken by CTA will be accessible by members of the wider in our galaxy. The improved spatial resolution and sensitivity of astronomical community, for the first time in this energy band. recent gamma-ray surveys of the Galactic plane have resolved This presentation will give an overview of CTA, and its proposed confusion of sources identified numerous sources to study the key science program. physics of particle acceleration and the diffusion of energetic particles into the galaxy. Here I highlight some recent studies of Submitted with the CTA Consortium Galactic accelerators from GeV to TeV energies, that allow us to 1 disentangle hadronic from leptonic emission, constrain cosmic ray Author(s): Reshmi Mukherjee diffusion, and measure the conditions of particle acceleration. Institution(s): 1. Barnard College, Columbia University Supernova remnants and pulsar wind nebulae are found to be the two most common Galactic sources identified in very high energy 401.02 – Spin-powered Pulsars in the CTA Era gamma rays, and the future capabilities of CTA promise a dramatic What can CTA do for the study of isolated and binary neutron increase in our knowledge of these classes which are currently stars? Are the recent Crab observations the vanguard of numerous limited to only a few of the most well-studied cases. strong pulsed detections in the CTA era? Will the typical pulsar show only the tail of the Fermi spectrum? Or will we be tantalized Author(s): John W. Hewitt1 by a handful of new unusual sources? I review our current HE Institution(s): 1. University of North Florida picture and suggest that pulsar binaries represent a new TeV frontier. 401.06 – Opportunities for Fundamental and New Physics with Very High Energy Gamma-ray Telescopes Author(s): Roger W. Romani1 Astronomical observations with the highest energy gamma rays Institution(s): 1. Stanford Univ. enable a wide range of fundamental physics measurements as well as searches for new physics beyond the Standard Model. In this 401.03 – Connection of Very High Energy Gamma-ray presentation, I will discuss indirect dark matter searches, Flares in Blazars to Activity at Lower Frequencies intergalactic magnetic field constraints, and tests of Lorentz The author will briefly review the results of multi-wavelength invariance with an emphasis on sensitivity gains that could be observations of blazars that emit very high-energy (VHE) gamma achieved with two new ground-based gamma-ray telescopes rays. The VHE gamma-ray emission is generally episodic, including operating at the TeV energy scale: the High-Altitude Water flares that are often very short-lived. While many of these flares Cherenkov observatory (HAWC) and the Cherenkov Telescope have counterparts only at X-ray energies, or no counterparts at all, Array (CTA). Multiwavelength and multimessenger observations some events are seen also at optical wavelengths, and a number are are an essential component of these studies needed to characterize associated with the passage of new superluminal knots passing the environments in which the highest energy gamma rays are through the core in mm-wave VLBA images. Two explanations for produced, the conditions encountered while traversing interstellar the short-term VHE flares in the relativistic jets are supersonic and intergalactic distances, and "conventional" astrophysical turbulence and ultra-fast plasma jets resulting from magnetic backgrounds. reconnections. Observations of frequency-dependent linear polarization during flares can potentially decide between these Author(s): Keith Bechtol1 models. VLBA images can help to locate VHE events that are seen Institution(s): 1. University of Wisconsin - Madison at millimeter wavelengths. In some cases, the flares take place near the parsec-scale core, while in others they occur closer to the black 401.07 – The Impact of CTA on Future Space-Based hole. High Energy Astrophysics Missions The Cherenkov Telescope Array will provide a great leap forward in the Early Universe scientific capability for Very High Energy (VHE) gamma-ray Deep studies of X-ray emission from galaxies, such as the Chandra astrophysics. In this talk I consider how the current observatory Deep Field-South 4 Ms (soon to be 7Ms) survey, have allowed us to design and future science return from CTA might influence the peer back in history at X-ray binary formation and evolution over science goals and design of future high energy astrophysics cosmic timescales. X-ray stacking observations of z=1-4 missions with a focus on the possibilities at gamma-ray energies. star-forming galaxies reveal that the metallicity evolution of the 1 Universe drives the evolution of the 2-10 keV X-ray luminosity per Author(s): Julie E. McEnery star formation rate (SFR), which is dominated by high mass X-ray Institution(s): 1. NASA's GSFC binaries (HMXBs). By studying local (z=0.02-0.2), rare, analogs of these high redshift galaxies, we have found further evidence that the X-ray emission per SFR is elevated compared to typical local 402 – Dark Matter, ISM, & Galaxies star-forming galaxies and this appears to be due to the lower metallicities of these galaxies. Theoretically, metal poor stars 402.01 – Recent Updates on the Searches for the 3.55 produce weaker stellar winds, which results in higher numbers of keV Line more massive binaries and therefore leads to higher X-ray The abundance of ubiquitous dark matter is now well quantified by luminosities in metal poor populations. We have performed an observations, yet its nature remains unknown. Dark matter is in-depth study of the only two local analogs that have spatially- believed to be composed primarily of an elementary particle. The resolved 2-10 keV emission with Chandra to present the bright end search for this particle is one of the major efforts in astrophysics of the X-ray luminosity distribution of HMXBs. Based on this and particle physics today. X-ray observations of dark matter study, we conclude that the X-ray luminosity functions in these dominated objects have the potential to reveal a signal from metal-poor galaxies differ from that of local star-forming galaxies. decaying or annihilating dark matter. We previously reported the Since galaxies at high redshifts (and their binaries) formed in a detection of an unidentified emission line at 3.55 keV in the more pristine universe, with few metals, the analogs that we have stacked XMM-Newton observations of galaxy clusters. The origin been studying offer cosmological insight about the heating of the of this unidentified line could be attributed to the decay of dark early Universe by HMXBs. matter particles. I will present the new results from the stacked Suzaku observations of galaxy clusters and provide a Author(s): Antara Basu-Zych2, Bret Lehmer5 , Ann E. comprehensive review on the detections and limits in the literature. Hornschemeier21 , Tassos Fragos , Andreas Zezas 3 , Mihoko Yukita42 , Andrew Ptak Author(s): Esra Bulbul1, Eric D. Miller11 , Mark W. Bautz Institution(s): 1. Geneva Observatory, 2. Goddard Space Flight Institution(s): 1. MIT Center, 3. Harvard- Smithsonian Center for Astrophysics, 4. Johns Hopkins University, 5. University of Arkansas 402.02 – A new deep, hard X-ray survey of M31: Identifying Black Holes and Neutron Stars in the 402.04 – The Circum-Galactic Medium of MASsive X-ray Binary Population of our Nearest Neighbor Spirals (CGM-MASS) I: Introduction to the X-ray binaries (XRBs) trace old and new stellar populations in XMM-Newton Large Project and a Case Study of NGC galaxies, and thus star formation history and star formation rate. 5908 X-ray emission from XRBs may be responsible for significant The Circum-Galactic Medium of MASsive Spirals (CGM-MASS) is a amounts of heating of the early Intergalactic Medium (IGM) at project studying the overall content, physical and chemical Cosmic Dawn and may also play a significant role in reionization. properties, and spatial distributions of the multi-phase circum- Until recently, the hard emission from these populations could galactic medium (CGM) around a small sample of the most massive only be studied for XRBs in our own galaxy, where it is often (M* >2×1011 M⊙ , vrot >300km/s) isolated spiral galaxies in the difficult to measure accurate distances and thus luminosities. The local Universe. In this talk, we will briefly introduce the sample and launch of NuSTAR, the first focusing hard X-ray observatory, has the science goals and present the first detailed case study of the allowed us to resolve the brightest XRBs (down to LX ~ few times XMM-Newton observation of the hot gas halo of NGC5908. After 10^38 erg/s) in galaxies like NGC 253, M83, and M82 up to 4 Mpc careful data calibration, point source removal, and background away. To reach much lower X-ray luminosities that are more typical analysis, we find the diffuse soft X-ray emission of NGC 5908 is of XRBs in the Milky Way (Lx <~ 10^37 erg/s), we have observed significantly more extended than the stellar light in the vertical M31 in 4 NuSTAR fields for more than 1 Ms total exposure, direction. The 0.5-1.25keV radial intensity profile tracing hot gas covering younger stellar population in a swath of the disk (within emission can be detected above the background out to ~2’, or the footprint of the Panchromatic Hubble Andromeda Treasury ~30kpc from the nucleus. The radial intensity distribution of hot (PHAT) Survey) and the older populations of the bulge. We detect gas can be characterized with a β-model with a core radius of 120 sources in the 4-25 keV band and over 40 hard band (12-25 rcore ~8.8kpc and the β-index of β~0.8. The spectra extracted from keV) accreting black holes and neutron stars, distinguished by their the inner halo indicates an extremely low metallicity of Z<0.1Z⊙ spectral shape in this band. The luminosity function (LF) of the and a temperature of kT~0.5keV. The cooling radius is hard band detected sources are compared to Swift/BAT-derived rcool ~27kpc or ~0.065r 200 , within which the hot gas could cool LFs of the Milky Way population, which reveals an excess of radiatively within the cosmic time. Using the best-fit models of the luminous sources in M31 when correcting for star formation rate spectra and the radial intensity profile, we further estimate some and stellar mass. We also discuss implications for this updated physical parameters of the hot gas and extrapolate them to larger understanding of XRB populations on early-Universe radii. Adding the mass of cold atomic and molecular gases, hot gas, measurements in, e.g., the 7 Ms Chandra Deep Field survey. and stars, the total baryon fraction fb200 within r is ~0.07, significantly below the cosmic baryon fraction of ~0.17. Therefore, Author(s): Daniel R. Wik4, Ann E. Hornschemeier4 , Mihoko ~60% of the baryons in the halo of NGC5908 is still “missing”. The Yukita448 , Andrew Ptak , Bret Lehmer , Thomas J. Maccarone 5 , hot gas accounts for ~56% of the total baryon content in the whole Vallia Antoniou29 , Andreas Zezas , Fiona Harrison 13 , Daniel Stern , halo, but only ~2% within the cooling radius. By comparing Tonia M. Venters4106 , Benjamin F. Williams , Michael Eracleous , NGC5908 to other galaxies or groups/clusters of galaxies, we find Paul P. Plucinsky27 , David A. Pooley that it could be slightly X-ray brighter at a given stellar mass, when Institution(s): 1. Caltech, 2. Harvard-Smithsonian Center for compared to lower-mass galaxies. NGC5908 also has fb Astrophysics, 3. Jet Propulsion Laboratory, 4. NASA Goddard comparable to the typical value of a galaxy group with a similar halo Space Flight Center, 5. Texas Tech University, 6. The Pennsylvania mass or rotation velocity. State University, 7. Trinity University, 8. University of Arkansas, 9. University of Crete, 10. University of Washington

402.03 – A Local Perspective on HMXB Populations in Author(s): Jiang-Tao Li4, Joel N. Bregman43 , Daniel Wang , 402.06 – Detecting the Missing Metals and Missing Robert A. Crain12 , Michael E. Anderson Baryons Through X-Ray Spectroscopy Institution(s): 1. Astrophysics Research Institute, Liverpool John About 90% of the metals produced in the universe and 50% of the Moores University, 2. Max-Planck Institute for Astrophysics, 3. baryons are unaccounted for through UV-IR and radio studies of University of Massachusetts, 4. University of Michigan stars and gas. This large amount of missing gas and metals likely lies in a hot phase (0.5-10x106 K) and must be enriched to about 402.05 – Dust Modeling of Si K Absorption in Galactic 0.2-0.3 of the solar metallicity, so it should be a good absorber of Bulge LMXBs with Chandra X-rays in the resonance lines of common elements. Both existing The Galactic Bulge hosts a large number of bright and highly data and simulations predict that hot galactic halos have N(H) absorbed low-mass X-ray binaries (LMXBs). Column densities ~1-10x1019 cm -2 and EW(OVII) = 3-10 mÅ, which are best studied between 1022 cm -2 and 5x10 23 cm -2 offer the opportunity and with instruments that can resolve the lines, as the estimated line contrast to study the Si K edge structure with very high spectral widths are 100-200 km/s. This sort of resolution and sensitivity is resolution. Recent models predict that the total extinction in X-ray possible with grating spectroscopy of the type envisioned for spectra not only involves X-ray absorption from gas and dust along missions such as Arcus and X-Ray Surveyor. These same the line of sight, but also significant contributions from dust instruments can probe the dynamics of the gas, and when applied scattering. A survey with the Chandra HETG of about a dozen to the halo of the Milky Way, can determine the rates of rotation LMXBs yields a rich variety of spectral features, showing that the Si and infall (or outflow) and the degree of turbulence. K edge structure is highly complex and variable, from source to source and with time for a given source. We find substructure from Author(s): Joel N. Bregman1, Matthew J. Miller1 , Edmund J. neutral atomic silicon, silicate dust absorption and scattering from Hodges-Kluck1 the interstellar medium (ISM), and Institution(s): 1. Univ. of Michigan superimposed ionized absorption signatures from the circumstellar environment of the LMXBs.

Author(s): Norbert S. Schulz1, Lia Corrales1 , Claude R 403 – Rapporteur Plenary Talk Canizares1 Institution(s): 1. MIT Authors Index Acosta Pulido, Jose: 106.25 Bird, Tony: 120.12 106.11 Diltz, Chris Scott.: 106.26 Agnew, Ryan: 120.33 Biretta, John A.: 100.01, 106.17 Carnerero Martin, Maria Isabel.: DiPompeo, Michael A.: 106.09 Akahori, Takuya: 111.03 Black, Christine: 106.09 106.25 Doty, John: 116.13 Al Noori, Hind: 114.17 Blackburn, Lindy: 301.02 Casandjian, Jean-Marc: 110.14 Drake, James: 101.05 Alford, Jason: 114.01 Blair, William P.: 118.08 Case, Gary L.: 118.09 Drake, Jeremy J.: 120.26 Aliotta, Paul H.: 116.03 Blanton, Elizabeth L.: 101.02 Chakrabarty, Deepto: 120.01, Drake, Stephen Alan.: 116.16 Allen, Glenn E.: 118.11 Bloser, Peter F.: 116.03, 116.04 120.18, 302.06 Drlica-Wagner, Alex: 110.08 Allen, Jessamyn: 120.01 Blundell, Katherine: 101.03 Charles, Eric: 110.08 Dubus, Guillaume: 120.08, Allured, Ryan: 116.02, 116.14 Bocchino, Fabrizio: 118.03 Chatterjee, Shami: 105.03 207.06 Alston, William: 106.19 Bodaghee, Arash: 120.03, Chatzikos, Marios: 111.04 Ducci, Lorenzo: 120.20 Alvarez Crespo, Nuria: 106.20 120.33 Chen, Chien-Ting J.: 106.18 Dunham, Michael M.: 120.16 Anderson, Craig: 110.04, 110.06 Boettcher, Markus: 106.10, Cherry, Michael L.: 118.09 Dutan, Ioana: 106.22 Anderson, Jay: 100.01, 106.17 106.14, 106.26, 106.32, 207.01 Cheung, Chi C.: 120.08, 207.06 Dwarkadas, Vikram: 118.04, Anderson, Matthew: 306.05 Bogdan, Akos: 111.08 Chiaberge, Marco: 100.01, 118.06, 118.07, 118.10 Anderson, Michael E.: 402.04 Bogdanov, Slavko: 105.03, 106.17 Echt, Olof: 116.03 Andrade-Santos, Felipe: 101.02 105.05, 120.04 Chiang, Chia-Ying: 120.07 Edelson, Rick: 106.05 Antoniou, Vallia: 110.02, Boggs, Steven E.: 106.18, Chomiuk, Laura: 207.06 Edwards, Philip: 120.08, 207.06 120.02, 120.26, 120.33, 402.02 120.03, 306.01 Christensen, Finn: 106.18, Eggen, Joseph R.: 106.04 Archibald, Anne M.: 120.04 Borkowski, Kazimierz J.: 120.03 Egron, Elise: 120.07 Archibald, Robert Frederic.: 118.02 Christensen, Nelson: 301.02 Eikenberry, Stephen S.: 109.01 114.02 Bostrom, Allison: 100.05 Christodoulou, Dimitris M.: Elvis, Martin: 106.02 Arenberg, Jonathan: 116.12 Bottacini, Eugenio: 106.27, 120.31 Enoto, Teruaki: 114.06 Arimoto, Makoto: 106.33 400.03 Churazov, Eugene: 101.01 Eracleous, Michael: 402.02 Arnaud, Keith A.: 115.02 Boyd, Patricia T.: 106.05, Civano, Francesca M.: 106.18 Esposito, Paolo: 120.20 Arzoumanian, Zaven: 105.06, 110.02, 120.29, 120.30, 120.32 Civitani, Marta M.: 116.02 Eufrasio, Rafael T.: 104.02 114.06, 302.01 Bozzo, Enrico: 113.03, 120.20 Clark, Peter: 106.16 Evans, Phil: 113.01, 120.20 Auchettl, Katie Amanda.: Brambilla, Gabriele: 114.05, Clarke, Tracy E.: 101.03, 111.04 Ezer, Cemile: 101.02 306.02 114.11 Clautice, Devon: 100.02, Fabbiano, Giuseppina: 106.02, Avachat, Sayali S.: 100.02, Brandt, Soren: 113.03 106.06 110.04, 110.06 106.11 Brandt, W. Niel.: 104.02, 106.18 Coe, Malcolm J.: 120.12, 207.06 Fabian, Andrew C.: 100.03, Ayres, Thomas R.: 117.03 Brazier, Adam: 105.03 Coley, Joel Barry.: 120.08, 101.03, 120.07, 120.14, 202.01, Bachetti, Matteo: 120.14, 207.03 Bregman, Joel N.: 110.05, 207.06 304.01 Baganoff, Frederick K.: 106.28, 110.12, 111.06, 203.04, 402.04, collaboration, MAGNET: 201.07 Falcone, Abraham: 106.31 110.02, 110.10 402.06 Collaboration, NuSTAR: 109.08 Falkner, Sebastian: 120.09, Bailey, Avery: 111.04 Breiding, Peter: 106.15 Collmar, Werner: 112.04 201.03, 201.08 Bailyn, Charles D.: 401.04 Breton, Rene: 114.17 Cominsky, Lynn R.: 113.04 Farnsworth, Damon: 111.04 Ballantyne, David R.: 106.08, Brickhouse, Nancy S.: 116.18 Connaughton, Valerie: 301.02, Fender, Rob P.: 109.01, 109.04 106.12, 108.01 Briggs, Michael Stephen.: 306.07 Feng, Hua: 120.05 Ballhausen, Ralf: 201.02 301.02, 306.07 Coppi, Paolo S.: 106.01, 401.04 Ferdman, Robert: 105.03, Balokovic, Mislav: 106.13 Brightman, Murray: 207.03 Corbel, Stephane: 109.04 114.02 Baring, Matthew G.: 105.04, Brooks, Alyson: 110.08 Corbet, Robin: 120.08, 120.12, Feroci, Marco: 302.06 106.14, 114.07, 304.05 Brorby, Matthew: 120.05 207.06 Ferrara, Elizabeth C.: 116.17 Barret, Didier: 120.07, 120.14 Brown, Alexander: 106.05 Corcoran, Michael F.: 306.04 Ferrigno, Carlo: 113.03, 201.03 Barsotti, Lisa: 301.01 Brown, Gregory: 115.01 Cordes, James M.: 105.03 Finger, Mark H.: 118.09 Barthelmy, Scott Douglas.: Brown, Shea: 111.04 Coriat, Mickael: 109.04 Forest, Cary: 300.02 106.33, 120.20 Bruccoleri, Alexander Robert.: Corrales, Lia: 110.10, 120.16, Forman, William R.: 101.01, Bartlett, Elizabeth: 120.12 116.10 120.22, 402.05 101.02, 111.07, 111.08 Bassa, Cees: 120.04 Brumback, McKinley: 120.06 Cotroneo, Vincenzo: 116.02, Fornasini, Francesca: 120.03 Basu-Zych, Antara: 104.02, Brunetti, Gianfranco: 101.04 116.14 Foster, Adam: 116.11, 116.18 402.03 Bucciantini, Niccolo: 118.01 Courvoisier, Thierry J-L.: 113.03 Fragos, Tassos: 104.01, 104.02, Bauer, Franz E.: 104.02, 118.06 Buckley, Matthew: 110.08 Craig, William W.: 106.18, 402.03 Bautz, Mark W.: 101.02, 111.10, Buisson, Douglas: 100.03 120.03 Frank, Kari A.: 118.04, 118.05 402.01 Bulbul, Esra: 101.02, 402.01 Crain, Robert A.: 402.04 Frechette, Eric: 120.33 Bayliss, Matthew: 101.02 Burderi, Luciano: 120.07 Crawford, Fronefield: 105.03 Freire, Paulo: 105.03 Bazzano, Angela: 113.03 Burke, Douglas J.: 110.04, Cuadra, Jorge: 109.07 Fruscione, Antonella: 110.04, Beardmore, Andrew P.: 114.02, 110.06 Cui, Xiaohong: 116.18 110.06 116.11 Burns, Eric: 301.02, 306.07 Cumbee, Renata: 117.05 Fryer, Chris: 103.02, 306.01 Bechtol, Keith: 401.06 Burrows, David N.: 118.04, D'Abrusco, Raffaele: 106.20 Fuerst, Felix: 120.24, 201.02, Becker, Peter A.: 120.09, 120.24, 118.05, 120.20 D'Ai, Antonino: 120.07 201.06, 201.07, 207.03 201.02, 201.08 Buxton, Michelle: 109.05, Dahlin, Patrick: 110.12 Fujita, Yutaka: 111.03 Behar, Ehud: 109.03 401.04 Dai, Lixin J.: 100.06 Fukumura, Keigo: 106.16, Beheshtipour, Banafsheh: Cackett, Edward: 120.07, 120.14, Dai, Xinyu: 111.06 109.03 202.04, 304.03 120.28 Dallilar, Yigit: 109.01 Gaensler, Bryan M.: 118.01 Beiersdorfer, Peter: 115.01 Cadonati, Laura: 205.01 Dalton, Matthew: 118.12 Galeazzi, Massimiliano: 117.04, Belmont, Renaud: 100.03 Cafmeyer, Julian: 110.05 Dauser, Thomas: 109.02, 201.03 200.04 Belyaev, Mikhail: 114.04, Camilo, Fernando: 105.03 de Geronimo, Gianluigi: 116.20 Gallo, Elena: 400.05 119.01 Camp, Jordan: 103.05, 301.02 De Nolfo, Georgia: 302.04 Gandhi, Poshak: 109.01 ben-Ami, Sagi: 116.14 Canizares, Claude R.: 402.05 Decourchelle, Anne: 118.03 Garcia, Javier: 109.02, 110.10, BenZvi, Segev: 306.03 Capellupo, Daniel M.: 106.28 Degenaar, Nathalie: 106.28 207.04 Betancourt-Martinez, Gabriele: Cappallo, Rigel: 120.31 Deller, Adam T.: 120.04 Garner, Alan: 109.01 115.01 Cappelluti, Nico: 400.02 Deneva, Julia S.: 105.03 Gaskins, Jennifer: 110.08 Bhattacharyya, Sudip: 120.07 Caputo, Regina: 110.08 Dhillon, Vik: 109.01 Gehrels, Neil: 106.05, 107.01, Binder, Breanna A.: 120.31 Cara, Mihai: 100.02, 106.06, Di Stefano, Rosanne: 207.02 114.02, 120.20 Gelfand, Joseph: 105.04, 114.07 Heinz, Sebastian: 111.09, 114.02, 114.06 Lin, Lin: 105.04 Gelino, Dawn M.: 106.05 303.01 Kato, Yuichi: 111.03 Lister, Matthew L.: 106.06 Gendreau, Keith C.: 302.01 Hell, Natalie: 115.01, 207.04 Kawai, Nobuyuki: 106.33 Littenberg, Tyson: 301.02 Gendron-Marsolais, Marie-Lou: Hemphill, Paul Britton.: 120.09, Kazanas, Demos: 106.06 Littlefair, Stuart: 109.01 101.03, 111.08 120.21, 120.24, 201.02, 201.03, Kazanas, Demosthenes: Liu, Jifeng: 207.02 Georganopoulos, Markos: 201.06 109.03, 112.01, 114.05, 114.11 Liu, Siming: 120.27 100.01, 100.02, 106.06, 106.11, Hendry, Doug: 106.16 Keane, Evan: 114.02 Liu, Wenhao: 117.04, 200.05 106.15, 106.17 Hertz, Edward: 116.02 Keek, Laurens: 106.12, 120.11 Lohfink, Anne: 100.03, Giglietto, Nicola: 107.02 Hessels, Jason: 105.03, 114.17, Kelley, Richard L.: 206.02 106.19 Gilfanov, Marat: 104.02 120.04 Kennea, Jamie: 110.02, 113.01, Long, Knox S.: 118.08 Gill, Ramandeep: 105.04, Hewitt, John W.: 401.05 114.02, 120.12, 120.20 Ludlam, Renee: 120.14 114.07 Hickox, Ryan C.: 106.09, Kim, Dong-Woo: 110.04, Luo, Bin: 104.02 Glikman, Eilat: 106.18 106.18, 400.01 110.06 Lynch, Ryan: 105.03 Gögüs, Ersin: 105.04 Hirsch, Maria: 207.04 Kinch, Brooks: 202.06 Lyons, David: 117.05 Gohil, Raj: 106.08 Hlavacek-Larrondo, Julie: King, Ashley L.: 102.01 Ma, Y. K.: 118.01 Goldstein, Adam: 301.02, 101.03, 111.08 Kippen, R. Marc.: 116.03 Maccarone, Thomas J.: 110.02, 306.07 Hodges-Kluck, Edmund J.: Kislat, Fabian: 116.20 120.31, 402.02 Gomez, Jose: 106.22 110.05, 110.12, 203.04, Klochkov, Dmitry: 120.21, Machacek, Marie E.: 101.01 Gonthier, Peter L.: 114.08 402.06 201.03, 201.04, 201.06 MacPherson, Emily: 401.04 Gorenstein, Paul: 103.06 Hogan, Brandon Scott.: 106.06 Kochanek, Christopher S.: Madsen, Erik: 105.03 Goronostaev, Mikhail: 120.21 Hogg, J. Drew: 120.10 111.06 Madsen, Kristin: 306.01 Gotthelf, Eric V.: 114.02, Hogge, Taylor: 111.04 Koh, Yew-Meng: 114.08 Madura, Thomas: 306.04 114.09, 117.01 Holder, Jamie: 106.30 Komossa, St.: 103.03 Mahmoodifar, Simin: 120.15, Gottlieb, Amy: 120.09, 120.24, Holland, Stephen: 112.02 Kopacek, Ondrej: 106.29 120.23 201.02 Holley-Bockelmann, Kelly: Kosak, Katie: 106.11 Majid, Walid A.: 114.16 Granot, Jonathan: 105.04, 301.04 Koss, Michael: 106.18 Makishima, Kazuo: 111.03 114.07 Holmes, Danika: 118.07 Koutroumpa, Dimitra: 110.14, Maksym, W. Peter.: 106.02 Grant, Catherine E.: 111.10 Homan, Jeroen: 109.05, 120.01, 117.04, 200.02 Malonis, Andrew: 116.13 Green, David: 118.02 120.07 Kouveliotou, Chryssa: 105.04, Malzac, Julien: 100.03 Grefenstette, Brian: 207.03, Hong, JaeSub: 120.26 114.07, 116.05 Marcu, Diana: 120.09 306.01, 306.04 Hoormann, Janie: 202.04 Kovar, Jiri: 106.29 Marcu-Cheatham, Diana: Grenier, Isabelle: 110.14 Hornschemeier, Ann E.: 104.02, Kraft, Ralph P.: 101.01, 111.08 120.24 Griffin, Rhiannon: 111.06 110.02, 207.03, 402.02, 402.03 Krawczynski, Henric: 116.20, Marcu-Cheatham, Diana Griffith, Christopher: 106.31 Hou, Meicun: 110.13 202.04 Monica.: 201.02 Grinberg, Victoria: 109.02, Howell, Steve B.: 106.05 Kretschmar, Peter: 201.03, Margutti, Raffaella: 103.01 201.06, 207.04 Hu, Chin-Ping: 114.10 201.06 Markevitch, Maxim L.: 101.04 Groh, Jose: 306.04 Huenemoerder, David: 117.02, Krimm, Hans A.: 106.33, 120.20 Markoff, Sera: 106.28 Gu, Liyi: 111.03 207.04 Krivonos, Roman: 120.03 Markowitz, Alex: 120.21 Guainazzi, Matteo: 116.11 Hunter, Stanley D.: 302.04, Krizmanic, John F.: 302.04 Marquez, Vanessa: 116.02 Guillot, Sebastien: 114.02 302.05 Krolik, Julian H.: 202.06 Marscher, Alan P.: 401.03 Gull, Theodore R.: 306.04 Huppenkothen, Daniela: Krumrey, Michael: 116.13 Marsh, Thomas: 109.01 Guo, Jincheng: 207.02 105.02, 105.04, 114.07 Krzanowski, James E.: 116.03 Marshall, Herman L.: 106.06 Gupta, Anjali: 100.04, 203.01 Hwang, Una: 118.02 Kühnel, Matthias: 120.09, Martin, Pierrick: 110.08, 207.06 GW follow-up team, Swift: Iaria, Rosario: 120.07 120.18, 120.21 Masetti, Nicola: 106.20 113.01 Ignace, Richard: 117.02 Kunneriath, Devaky: 106.29 Massaro, Francesco: 106.20 Gwynne, Peter: 118.02 Intema, Huib: 101.03 Kuntz, K. D.: 117.04, 118.08, Mathur, Smita: 100.04 Haberl, Frank: 116.11, 120.12, Isler, Jedidah: 401.04 200.03, 200.06 Maune, Jeremy: 106.04 120.26 Iwanicki, Allana: 118.11 KUNTZ, Kip: 110.14 McBride, Vanessa: 120.08, Haggard, Daryl: 106.28 Jackson, Brenton: 120.33 Kuulkers, Erik: 113.03 120.12, 207.06 Hailey, Charles James.: 106.18, Jackson, Tom: 116.14 Lallement, Rosine: 110.14 McClintock, Jeffrey E.: 109.02 120.03 Jahoda, Keith: 116.05 LaMarr, Beverly: 116.13 McCollough, Michael L.: 110.04, Hainline, Kevin Nicholas.: Jaodand, Amruta: 120.04 LaMassa, Stephanie M.: 106.18 110.06, 120.16 106.09 Jenke, Peter: 118.09 Lamb, Frederick K.: 120.13 McConnell, Mark L.: 112.04, Halpern, Jules P.: 114.09, Ji, Li: 120.27 Landoni, Marco: 106.20 116.03, 116.04 120.04 Johnson, Ryan: 101.02 Lansbury, George: 106.18 McDonald, Michael: 111.10 Hamaguchi, Kenji: 306.04 Johnston, Simon: 118.12 Laubis, Christian: 116.13 McEnery, Julie E.: 401.07 Hamann, Wolf-Rainer: 117.02 Jones, Christine: 101.01, 101.02, Lauer, Jennifer L.: 110.04, McEntaffer, Randall L.: 116.19 Hanlon, Lorraine: 113.03 111.07, 111.08 110.06 McLaughlin, Maura: 105.03, Hanu, Andrei R.: 302.04 Jones, Mackenzie L.: 106.09 Laurent, Philippe: 113.03 114.17 Hardee, Philip E.: 106.22 Jones, Thomas W.: 101.04 Laycock, Silas: 120.12, 120.31 McLin, Kevin M.: 113.04 Harding, Alice Kust.: 105.04, Jordan, Zachary: 120.33 Lazarus, Patrick: 105.03 Meli, Athina: 106.22 114.05, 114.07, 114.08, 114.11, Jorstad, Svetlana G.: 401.03 Lebrun, François: 113.03 Mereghetti, Sandro: 113.03 118.09, 207.01 Jourdain, Elisabeth: 109.10 Legere, Jason S.: 116.03, 116.04 Mesinger, Andrei: 104.04 Harris, Daniel E.: 106.11 Kaaret, Philip: 120.05, 203.05 Lehmer, Bret: 104.02, 110.02, Meyer, Eileen: 100.02, 106.15, Harrison, Fiona: 106.13, 106.18, Kalapotharakos, Constantinos: 402.02, 402.03 106.17 114.02, 120.03, 120.14, 120.25, 114.11 Lehner, Luis: 306.05 Meyer, Eileen T.: 100.01 207.03, 306.01, 402.02 Kalapotharakos, Constantions: Leutenegger, Maurice A.: Miceli, Marco: 118.03 Hartmann, Dieter: 106.22, 114.05 115.01, 207.04 Mihara, Tatehiro: 106.33 108.02 Kallman, Timothy R.: 116.05 Li, Hui: 106.10 Miles, Drew M.: 116.22 Hasan, Imran: 401.04 Kalogera, Vassiliki: 104.02 Li, Jiang-Tao: 118.03, 402.04 Milisavljevic, Dan: 106.20 Hays, Elizabeth A.: 116.21, Kara, Erin: 100.06, 202.03 Li, kunyang: 106.11 Miller, Eric: 101.02, 116.11 118.09 Karas, Vladimir: 106.29 Li, Xiang-Dong: 120.27 Miller, Eric D.: 111.10, 402.01 Hegley, Jakob: 107.01 Kargaltsev, Oleg: 105.04, 114.07 Li, Zhiyuan: 110.13 Miller, Hugh R.: 106.04 Heilmann, Ralf K.: 116.10 Karovska, Margarita: 106.02 Liebling, Steven: 306.05 Miller, Jon M.: 100.05, 100.06, Heinke, Craig O.: 106.28 Kaspi, Victoria M.: 105.03, Lin, Dacheng: 120.07 120.07, 120.14, 120.25, 300.03 Miller, M. Coleman.: 120.07, Peacock, Mark: 120.19 Roustazadeh, Parisa: 106.32 Stelter, R. Deno: 109.01 120.13, 120.17 Peris, Charith: 109.06 Rudnick, Lawrence: 111.04 Stern, Daniel: 106.18, 106.24, Miller, Matthew J.: 203.04, Perlman, Eric S.: 100.01, Russell, Christopher Michael 114.02, 120.03, 402.02 402.06 100.02, 106.06, 106.11, 106.17, Post.: 109.07, 306.04 Stevens, Abigail L.: 105.01 Miller, Neal A.: 400.04 106.30 Ruszkowski, Mateusz: 110.03 Stevens, Jamie: 120.08, 207.06 Mineo, Stefano: 104.02 Peruta, Carolyn: 113.04 Ryan, James M.: 116.04 Stone, James Mclellan.: 119.01 Mirabel, I. Felix.: 120.05 Petre, Robert: 118.02, 206.03 Ryu, Dongsu: 101.04 Storchi-Bergmann, Thaisa: Mitsuda, Kazuhisa: 206.02 Phillipson, Rebecca: 120.30, Sadowski, Aleksander: 202.05 106.02 Miyasaka, Hiromasa: 306.01 120.32 Saitoh, Shinya: 106.01 Strader, Jay: 207.06 Mizuno, Yosuke: 106.22 Pinto, Ciro: 106.19 Sakamoto, Takanori: 106.33, Strohmayer, Tod E.: 120.15, Moffat, Anthony F J.: 306.04 Pittard, Julian: 306.04 107.01 120.23 Moiseev, Alexander: 116.08 Pivovaroff, Michael: 114.02 Salmaso, Bianca: 116.02 Strong, Andrew: 107.02 Mooley, Kunal: 109.01 Plucinsky, Paul P.: 116.11, Salvo, Tiziana: 120.07 Stuchlik, David: 116.20 Moran, Edward C.: 106.07 402.02 Santander, Marcos: 107.03 Stuhlinger, Martin: 116.11, Morgan, Douglas: 110.04, Pohl, Martin: 106.22 Sapkota, Dhaka Mohan.: 306.04 110.06 Pollock, Andrew: 116.11 116.06 Su, Yuanyuan: 101.01 Mori, Kaya: 120.03 Ponti, Gabriele: 106.28, 109.04 Sarazin, Craig L.: 101.02, 111.04 Suchy, Slawomir: 120.09 Morsony, Brian J.: 111.09 Pooley, David A.: 402.02 Savchenko, Volodymyr: 113.03 Summerlin, Errol J.: 106.14 Moskalenko, Igor V.: 107.02 Pooley, Guy G.: 109.06 Schattenburg, Mark: 116.10 Sundqvists, Jon O.: 207.04 Mossman, Amy: 110.04, 110.06 Porter, Frederick S.: 115.01 Schlitz, Joseph: 107.01 Sushch, Iurii: 118.12 Motl, Patrick M.: 306.05 Postnov, Konstantin: 120.21 Schneider, Donald P.: 104.02 Swisdak, M.: 101.05 Motta, Sara: 109.04 Pottschmidt, Katja: 110.02, Schnittman, Jeremy: 202.06, Takada, Atsushi: 116.09 Mueller, Guido: 301.05 120.09, 120.21, 120.24, 201.02, 304.02 Takahashi, Hiromitsu: 306.04 Mukai, Koji: 206.03 201.03, 201.06, 207.04 Scholz, Paul: 105.03 Takahashi, Masaaki: 106.16 Mukherjee, Reshmi: 401.01 PRAXyS Team, The: 116.05 Scholze, Frank: 116.13 Takahashi, Tadayuki: 206.01 Mullen, Patrick: 117.05 Prestwich, Andrea H.: 120.05 Schultz, David R.: 117.05 Takizawa, Motokazu: 111.03 Murray, Stephen S.: 101.02 Prigozhin, Gregory: 116.13 Schulz, Norbert S.: 117.02, Tan, William: 118.11 Mushotzky, Richard: 106.05, Primini, Francis A.: 207.02 120.01, 207.04, 402.05 Tananbaum, Harvey: 116.14 400.04 Proga, Daniel: 300.01 Schwanke, Ullrich: 118.12 Tanimori, Toru: 116.09 M\'endez, Mariano: 120.27 Ptak, Andrew: 110.02, 207.03, Schwarm, Fritz-Walter: 120.24, Taylor, Gregory B.: 101.03 Nakahira, Satoshi: 106.33 402.02, 402.03 201.02, 201.03, 201.08 Temim, Tea: 118.01 Nakazawa, Kazuhiro: 111.03 Racusin, Judith L.: 112.01, Schwartz, Daniel A.: 116.14 Tendulkar, Shriharsh P.: 114.02, Natalucci, Lorenzo: 113.03, 301.02 Sembay, Steve: 116.11 207.03 120.14 Rafikov, Roman R.: 119.01 Serino, Motoko: 106.33 The SMC XVP Collaboration, &: Neilsen, David: 306.05 Rahoui, Farid: 109.05, 120.03 Seymour, Andrew: 105.03 120.26 Neilsen, Joseph: 106.28, Raino', Silvia: 107.02 Sharma, Neetika: 306.04 Thorpe, James: 301.03 109.04, 109.05 Raiteri, Claudia Maria.: 106.25 Shawhan, Peter S.: 301.02 Thrush, Samantha: 106.32 neilson, hilding: 117.02 Rana, Vikram: 120.14 Shelton, Robin L.: 117.05, Timokhin, Andrey: 114.05, Ng, Chi Yung: 118.01, 306.02 Ranalli, Piero: 104.02 203.03 302.04 Ng, Chi-Yung: 114.10 Randall, Scott W.: 101.01, Shemmer, Ohad: 104.02 Tobler, Jennifer: 112.02 Niemiec, Jacek: 106.22 101.02, 111.07, 111.08 Shenar, Tomer: 117.02 Tombesi, Francesco: 106.06, Nishikawa, Ken-Ichi: 106.22 Ransom, Scott M.: 105.03 Shirazi, Farzane: 116.03 106.16, 109.03, 400.06 Noble, Scott: 202.06 Rappaport, Saul A.: 111.10 Shrader, Chris R.: 106.03, Tomsick, John: 114.02, 120.03, Nordlund, Aake: 106.22 Ray, Paul S.: 105.06, 302.06 109.03 120.14, 120.33, 202.02 Norman, Colin Arthur.: 100.01, Reddy, Ratuja: 118.06 Simionescu, Aurora: 111.03 Torpin, Trevor: 120.29 106.17 Reeves, James: 400.06 Simonnet, Aurore: 113.04 Townsend, Lee: 120.12, 207.06 Nowak, Michael: 106.28, Reid, Paul B.: 116.02, 116.14 Singer, Leo Pound.: 301.02, Townsend, Richard D.: 207.04 120.18, 207.04 Remillard, Ronald A.: 109.02, 306.06 Tozzi, Paolo: 104.02 Nugent, Jenna: 111.06 109.06, 116.13, 207.05, 302.02 Slane, Patrick O.: 118.01, 306.02 Treister, Ezequiel: 106.18 Nulsen, Paul: 101.01, 111.07, Reynolds, Christopher S.: Slany, Petr: 106.29 Trier Frederiksen, Jacob Trier.: 111.08 100.06, 101.05, 106.19, 111.09, Smale, Alan P.: 116.16, 120.29, 106.22 O'Brien, P. T.: 112.03, 116.01 115.01, 120.10, 400.06 120.30, 120.32 Trinchieri, Ginevra: 110.04, O'Sullivan, Ewan: 110.04, Reynolds, Stephen P.: 118.02, Smith, Evan: 106.30 110.06 110.06 306.01 Smith, Howard Alan.: 106.20 Trolier-McKinstry, Susan: Oda, Ryoma: 106.33 Ricarte, Angelo: 106.18 Smith, Krista Lynne.: 106.05, 116.02, 116.14 Oh, Siang P.: 101.04 Ricci, Claudio: 106.18 400.04 Trump, Jonathan R.: 104.02 Okajima, Takashi: 107.01, Ricci, Federica: 106.20 Smith, Randall K.: 101.02, Tsavalas, John G.: 116.03 116.20 Richardson, Noel: 306.04 110.09, 116.18, 120.22, 302.03 Ubertini, Pietro: 113.03 Orlando, Elena: 107.02, Rivers, Elizabeth: 106.23 Snowden, Steve L.: 200.03 Urry, C. Megan.: 106.18, 401.04 107.04 Roberg-Clark, Gareth: 101.05 Snowden, Steven L.: 110.14 Ursino, Eugenio: 117.04 Oskinova, Lidia: 117.02 Roberts, Mallory: 114.17 Sohn, S. Tony: 100.01, 106.17 Uttley, Phil: 105.01 Owen, Frazer N.: 106.11 Roberts, Oliver: 105.04 Sol, Helene: 106.22 Valencic, Lynne A.: 110.09, Owocki, Stan: 306.04 Rodriguez, Jerome: 109.06 Sparks, William B.: 100.01, 120.22, 120.29 Oya, Igor: 118.12 Roediger, Elke: 101.01, 111.08 106.11, 106.17 van der Horst, Alexander: Page, Kim L.: 110.02 Romani, Roger W.: 114.14, Spitler, Laura: 105.03 105.04 Paggi, Alessandro: 106.02, 304.06, 401.02 Sschoenherr, Gabriele: 201.03 van der Klis, Michiel: 105.01 106.20, 110.04, 110.06 Romano, Patrizia: 106.25, Stairs, Ingrid H.: 105.03 Van Der Marel, Roeland P.: Palenzuela, Carlos: 306.05 120.20 Stancil, Phillip C.: 117.05 100.01, 106.17 Pannuti, Thomas: 118.11 Romero-Canizales, Cristina: Stappers, Benjamin: 105.03 van Leeuwen, Joeri: 105.03 Pareschi, Giovanni: 116.02 118.06 Staubert, Rüdiger: 120.21, Van Weeren, Reinout J.: 111.04 Parker, Michael: 120.07, 120.14 Roming, Peter: 112.02 201.05, 201.06 Varniere, Peggy: 109.06 Patel, Chitrang: 105.03 Roques, Jean-Pierre: 109.10, Stawarz, Lukasz: 106.01 Vasilopoulos, Georgios: 120.12 Paterno-Mahler, Rachel: 101.02 113.03 Stecker, Floyd W.: 302.04 Veilleux, Sylvain: 111.10, 400.06 Pavlov, George G.: 105.04 Rothschild, Richard E.: 120.21, Steiner, James F.: 109.02, Veitch, John: 301.02 Pe'er, Asaf: 106.22 201.06 109.06, 120.31, 207.05 Venter, Christo: 207.01 Venters, Tonia M.: 302.04, Wang, Na: 120.27 120.09, 120.24, 201.01, Yukita, Mihoko: 104.02, 402.02 Wasti, Sambid K.: 116.04 201.02, 201.08 110.02, 207.03, 402.02, 402.03 Vercellone, Stefano: 106.25, Watanabe, Ken: 107.01 Wong, B.T.T.: 306.02 Yusef-Zadeh, Farhad: 106.28 120.20 Watts, Anna: 105.04 Wong, Emily N.: 116.03 Zepf, Steve E.: 120.19 Vignali, Cristian: 104.02 Weidenspointner, Georg: 113.03 Wood, Kent: 120.24 Zezas, Andreas: 104.02, 110.02, Vikhlinin, Alexey: 116.02, 116.14 Weiner, Ori: 306.08 Wood, Kent S.: 120.09, 201.02 120.02, 120.26, 120.33, 207.03, Villata, Massimo: 106.25 Wiggins, Brandon: 110.11 Wood, Matthew: 110.08 402.02, 402.03 Vink, Jacco: 118.03 Wik, Daniel R.: 110.02, 111.04, Wright, Nick: 120.26 Zhang, Binbin: 301.02 Vogel, Stuart N.: 400.04 402.02 Wu, Jianfeng: 400.05 Zhang, Haocheng: 106.10, Vrtilek, Saeqa Dil.: 109.06 Willett, Rebecca: 118.02 Xue, Yongquan: 104.02 106.26 Vydra, Ekaterina: 107.01 Williams, Benjamin F.: 402.02 Yan, Shu-Ping: 120.27 Zhang, William: 106.18, 120.03 Wadiasingh, Zorawar: 207.01 Wilms, Joern: 110.10, 120.09, Yang, Hsiang-Yi Karen: 110.03 Zhang, Xiao-Ling: 118.09 Wallace, Margeaux L.: 116.02, 120.18, 120.21, 120.24, 201.02, Yang, Jun: 120.31 Zhu, Weiwei: 105.03 116.14 201.03, 201.06, 201.08, 207.04 Yaqoob, Tahir: 106.18 Zoghbi, Abderahmen: 120.25 Walton, Dom: 109.08, 207.03 Wilson, Lynn: 101.04 Yoshida, Atsumasa: 106.33 Zoglauer, Andreas: 306.01 Wang, Daniel: 109.07, 109.09, Wilson-Hodge, Colleen A.: Younes, George A.: 105.04, Zweibel, Ellen Gould.: 110.03 203.02, 402.04 118.09, 302.06 114.07 Wang, Junfeng: 106.02 Winkler, P. Frank.: 118.08 Yuan, Qiang: 109.09 Wang, JunXian: 104.02 Wolff, Michael Thomas.: Yuasa, Takayuki: 306.04